Manual

User Manual:

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I Using the Pencil Code
II Programming the Pencil Code
III Appendix
IV Indexes

The Pencil Code:

A High-Order MPI code for MHD Turbulence

User’s and Reference Manual

December 23, 2018

http://www.nordita.org/software/pencil-code/

https://github.com/pencil-code/pencil-code

The PENCIL CODE: multi-purpose and multi-user maintained

http://www.nordita.org/~brandenb/talks/misc/PencilCode04.htm

Figure 1: Check-in patterns as a function of time for different subroutines. The different users are marked

by different symbols and different colors.

Contributors to the code

(in inverse alphabetical order according to their user name)

An up to date list of Pencil Code contributors can be found at GitHub.

wladimir.lyra Wladimir Lyra California State University/JPL

weezy S. Louise Wilkin University of Newcastle

wdobler Wolfgang Dobler Potsdam

vpariev Vladimir Pariev University of Rochester

torkel Ulf Torkelsson Chalmers University

tavo.buk Gustavo Guerrero Stanford University

thomas.gastine Thomas Gastine MPI for Solar System Research

theine Tobias (Tobi) Heinemann IAS Princeton

tarek Tarek A. Yousef University of Trondheim

sven.bingert Sven Bingert MPI for Solar System Research

steveb Steve Berukoff UCLA

snod Andrew Snodin University of Newcastle

pkapyla Petri K¨

apyl¨

a University of Helsinki

nils.e.haugen Nils Erland L. Haugen SINTEF

ngrs Graeme R. Sarson University of Newcastle

NBabkovskaia Natalia Babkovskaia University of Helsinki

mreinhardt Matthias Rheinhardt University of Helsinki

mkorpi Maarit J. K¨

apyl¨

a (n´

ee Korpi, Mantere) University of Helsinki

miikkavaisala Miikka V¨

ais¨

al¨

a University of Helsinki

mee Antony (tOnY) Mee University of Newcastle

mcmillan David McMillan York University, Toronto

mattias Mattias Christensson formerly at Nordita

koenkemel Koen Kemel Nordita, Stockholm

karlsson Torgny Karlsson Nordita

joishi Jeff S. Oishi Kavli Institute for Particle Astrophysics

joern.warnecke J¨

orn Warnecke MPI for Solar System Research, Lindau

Iomsn1 Simon Candelaresi University of Dundee, Dundee

fadiesis Fabio Del Sordo Nordita, Stockholm

dorch Bertil Dorch University of Copenhagen

boris.dintrans Boris Dintrans Observatoire Midi-Pyr´

en´

ees, Toulouse

dhruba.mitra Dhrubaditya Mitra Nordita, Stockholm

ccyang Chao-Chin Yang Lund Observatory

christer Christer Sandin University of Uppsala

Bourdin.KIS Philippe Bourdin MPI for Solar System Research

AxelBrandenburg Axel Brandenburg Nordita

apichat Apichat Neamvonk University of Newcastle

amjed Amjed Mohammed University of Oldenburg

alex.i.hubbard Alex Hubbard Am. Museum Nat. History

michiel.lambrechts Michiel Lambrechts Lund Observatory, Lund University

anders Anders Johansen Lund Observatory, Lund University

mppiyali Piyali Chatterjee University of Oslo

2001–2017 Wolfgang Dobler & Axel Brandenburg

Permission is granted to make and distribute verbatim copies of this manual provided

the copyright notice and this permission notice are preserved on all copies.

iii

Permission is granted to copy and distribute modiﬁed versions of this manual under

the conditions for verbatim copying, provided that the entire resulting derived work is

distributed under the terms of a permission notice identical to this one.

License agreement and giving credit

The content of all ﬁles under :pserver:$USER@svn.nordita.org:/var/cvs/brandenb are

under the GNU General Public License (http://www.gnu.org/licenses/gpl.html).

We, the PENCIL CODE community, ask that in publications and presenta-

tions the use of the code (or parts of it) be acknowledged with reference to

the web site http://www.nordita.org/software/pencil-code/ or (equivalently) to.

https://github.com/pencil-code/pencil-code. As a courtesy to the people involved in

developing particularly important parts of the program (use svn annotate src/*.f90 to

ﬁnd out who did what!) we suggest to give appropriate reference to one or several of the

following (or other appropriate) papers (listed here in temporal order):

Dobler, W., Haugen, N. E. L., Yousef, T. A., & Brandenburg, A.: 2003, “Bottleneck ef-

fect in three-dimensional turbulence simulations,” Phys. Rev. E 68, 026304, 1-8

(astro-ph/0303324)

Haugen, N. E. L., Brandenburg, A., & Dobler, W.: 2003, “Is nonhelical hydromag-

netic turbulence peaked at small scales?” Astrophys. J. Lett. 597, L141-L144

(astro-ph/0303372)

Brandenburg, A., K ¨

apyl¨

a, P., & Mohammed, A.: 2004, “Non-Fickian diffusion and

tau-approximation from numerical turbulence,” Phys. Fluids 16, 1020-1027

(astro-ph/0306521)

Johansen, A., Andersen, A. C., & Brandenburg, A.: 2004, “Simulations of dust-

trapping vortices in protoplanetary discs,” Astron. Astrophys. 417, 361-371

(astro-ph/0310059)

Haugen, N. E. L., Brandenburg, A., & Mee, A. J.: 2004, “Mach number dependence

of the onset of dynamo action,” Monthly Notices Roy. Astron. Soc. 353, 947-952

(astro-ph/0405453)

Brandenburg, A., & Multam ¨

aki, T.: 2004, “How long can left and right handed life forms

coexist?” Int. J. Astrobiol. 3, 209-219 (q-bio/0407008)

McMillan, D. G., & Sarson, G. R.: 2005, “Dynamo simulations in a spherical shell of

ideal gas using a high-order Cartesian magnetohydrodynamics code,” Phys. Earth

Planet. Int.153, 124-135

Heinemann, T., Dobler, W., Nordlund, ˚

A., & Brandenburg, A.: 2006, “Radiative transfer

in decomposed domains,” Astron. Astrophys. 448, 731-737 (astro-ph/0503510)

Dobler, W., Stix, M., & Brandenburg, A.: 2006, “Convection and magnetic ﬁeld genera-

tion in fully convective spheres,” Astrophys. J. 638, 336-347 (astro-ph/0410645)

Snodin, A. P., Brandenburg, A., Mee, A. J., & Shukurov, A.: 2006, “Simulating ﬁeld-

aligned diffusion of a cosmic ray gas,” Monthly Notices Roy. Astron. Soc. 373, 643-

652 (astro-ph/0507176)

Johansen, A., Klahr, H., & Henning, T.: 2006, “Dust sedimentation and self-sustained

Kelvin-Helmholtz turbulence in protoplanetary disc mid-planes,” Astrophys. J.

636, 1121-1134 (astro-ph/0512272)

de Val-Borro, M. and 22 coauthors (incl. Lyra, W.): 2006, “A comparative study

of disc-planet interaction,” Monthly Notices Roy. Astron. Soc. 370, 529-558

(astro-ph/0605237)

Johansen, A., Oishi, J. S., Mac Low, M. M., Klahr, H., Henning, T., & Youdin, A.: 2007,

“Rapid planetesimal formation in turbulent circumstellar disks,” Nature 448,

1022–1025 (arXiv/0708.3890)

Lyra, W., Johansen, A., Klahr, H., & Piskunov, N.: 2008, “Global magnetohydrody-

namical models of turbulence in protoplanetary disks I. A cylindrical potential

on a Cartesian grid and transport of solids,” Astron. Astrophys. 479, 883-901

(arXiv/0705.4090)

Brandenburg, A., R ¨

adler, K.-H., Rheinhardt, M., & K ¨

apyl¨

a, P. J.: 2008, “Magnetic diffu-

sivity tensor and dynamo effects in rotating and shearing turbulence,” Astrophys.

J. 676, 740-751 (arXiv/0710.4059)

Lyra, W., Johansen, A., Klahr, H., & Piskunov, N.: 2008, “Embryos grown in the dead

zone. Assembling the ﬁrst protoplanetary cores in low-mass selfgravitating cir-

cumstellar disks of gas and solids,” Astron. Astrophys. 491, L41-L44

Lyra, W., Johansen, A., Klahr, H., & Piskunov, N.: 2009, “Standing on the shoulders of

giants. Trojan Earths and vortex trapping in low-mass selfgravitating protoplan-

etary disks of gas and solids,” Astron. Astrophys. 493, 1125-1139

Lyra, W., Johansen, A., Zsom, A., Klahr, H., & Piskunov, N.: 2009, “Planet formation

bursts at the borders of the dead zone in 2D numerical simulations of circumstel-

lar disks,” Astron. Astrophys. 497, 869-888 (arXiv/0901.1638)

Mitra, D., Tavakol, R., Brandenburg, A., & Moss, D.: 2009, “Turbulent dynamos in spher-

ical shell segments of varying geometrical extent,” Astrophys. J. 697, 923-933

(arXiv/0812.3106)

Haugen, N. E. L., & Kragset, S.: 2010, “Particle impaction on a cylinder in a crossﬂow

as function of Stokes and Reynolds numbers,” J. Fluid Mech. 661, 239-261

Rheinhardt, M., & Brandenburg, A.: 2010, “Test-ﬁeld method for mean-ﬁeld coefﬁcients

with MHD background,” Astron. Astrophys. 520, A28 (arXiv/1004.0689)

Babkovskaia, N., Haugen, N. E. L., Brandenburg, A.: 2011, “A high-order public domain

code for direct numerical simulations of turbulent combustion,” J. Comp. Phys.

230, 1-12 (arXiv/1005.5301)

Johansen, A., Klahr, H., & Henning, Th.: 2011, “High-resolution simulations of planetes-

imal formation in turbulent protoplanetary discs,” Astron. Astrophys. 529, A62

Johansen, A., Youdin, A. N., & Lithwick, Y.: 2012, “Adding particle collisions to the for-

mation of asteroids and Kuiper belt objects via streaming instabilities,” Astron.

Astrophys. 537, A125

Lyra, W. & Kuchner, W. : 2013, “Formation of sharp eccentric rings in debris disks with

gas but without planets,” Nature 499, 184–187

Yang, C.-C., & Johansen, A.: 2016, “Integration of Particle-Gas Systems with Stiff Mu-

tual Drag Interaction,” Astrophys. J. Suppl. Series 224, 39

This list is not always up-to-date. We therefore ask the developers to check in new rele-

vant papers, avoiding however redundancies.

Foreword

This code was originally developed at the Turbulence Summer School of the Helmholtz

Institute in Potsdam (2001). While some SPH and PPM codes for hydrodynamics and

magnetohydrodynamics are publicly available, this does not generally seem to be the

case for higher order ﬁnite-difference or spectral codes. Having been approached by peo-

ple interested in using our code, we decided to make it as ﬂexible as possible and as

user-friendly as seems reasonable, and to put it onto a public

CVS

repository. Since

21 September 2008 it is distributed via https://github.com/pencil-code/pencil-code.

The code can certainly not be treated as a black box (no code can), and in order to solve

a new problem in an optimal way, users will need to ﬁnd their own optimal set of pa-

rameters. In particular, you need to be careful in choosing the right values of viscosity,

magnetic diffusivity, and radiative conductivity.

The PENCIL CODE is primarily designed to deal with weakly compressible turbulent

ﬂows, which is why we use high-order ﬁrst and second derivatives. To achieve good par-

allelization, we use explicit (as opposed to compact) ﬁnite differences. Typical scientiﬁc

targets include driven MHD turbulence in a periodic box, convection in a slab with non-

periodic upper and lower boundaries, a convective star embedded in a fully nonperiodic

box, accretion disc turbulence in the shearing sheet approximation, etc. Furthermore,

nonlocal radiation transport, inertial particles, dust coagulation, self-gravity, chemical

reaction networks, and several other physical components are installed, but this num-

ber increases steadily. In addition to Cartesian coordinates, the code can also deal with

spherical and cylindrical polar coordinates.

Magnetic ﬁelds are implemented in terms of the magnetic vector potential to ensure

that the ﬁeld remains solenoidal (divergence-free). At the same time, having the mag-

netic vector potential readily available is a big advantage if one wants to monitor the

magnetic helicity, for example. The code is therefore particularly well suited for all kinds

of dynamo problems.

The code is normally non-conservative; thus, conserved quantities should only be con-

served up to the discretization error of the scheme (not to machine accuracy). There is

no guarantee that a conservative code is more accurate with respect to quantities that

are not explicitly conserved, such as entropy. Another important quantity that is (to

our knowledge) not strictly conserved by ordinary ﬂux conserving schemes is

magnetic

helicity

There are currently no plans to implement adaptive mesh reﬁnement into the code,

which would cause major technical complications. Given that turbulence is generically

space-ﬁlling, local reﬁnement to smaller scales would often not be very useful anyway.

On the other hand, in some geometries turbulence may well be conﬁned to certain re-

gions in space, so one could indeed gain by solving the outer regions with fewer points.

In order to be cache-efﬁcient, we solve the equations along

pencils

in the xdirection.

One very convenient side-effect is that auxiliary and derived variables use very little

memory, as they are only ever deﬁned on one pencil. The domain can be tiled in the y

and zdirections. On multiprocessor computers, the code can use

MPI

(Message Pass-

ing Interface) calls to communicate between processors. An easy switching mechanism

allows the user to run the code on a machine without MPI libraries (e.g. a notebook

computer). Ghost zones are used to implement boundary conditions on physical and

processor boundaries.

vii

A high level of ﬂexibility is achieved by encapsulating individual physical processes

and variables in individual

modules

, which can be switched on or off in the ﬁle

‘Makefile.local’ in the local ‘src’ directory. This approach avoids the use of difﬁcult-

to-read preprocessor directives, at the price of requiring one dummy module for each

physics module. For nonmagnetic hydrodynamics, for example, one will use the module

‘nomagnetic.f90’ and speciﬁes

MAGNETIC = nomagnetic

in ‘Makefile.local’, while for MHD simulations, ‘magnetic.f90’ will be used:

MAGNETIC = magnetic

Note that the term

module

as used here is only loosely related to Fortran modules: both

‘magnetic.f90’ and ‘nomagnetic.f90’ deﬁne an F90 module named Magnetic — this is the

basis of the switching mechanism we are using.

Input parameters (which are set in the ﬁles ‘start.in’, ‘run.in’) can be changed without

recompilation. Furthermore, one can change the list of variables for monitoring (diag-

nostic) output on the ﬂy, and there are mechanisms for making the code reload new

parameters or exit gracefully at runtime. You may want to check for correctness of these

ﬁles with the command pc_configtest.

The requirements for using the Pencil-MPI code are modest: you can use it on any Linux

or Unix system with a

F95

and

compiler suite, like

GNU gcc

and

gfortran

, together

with the shell

CSH

, and the

Perl

interpreter are mandatory requirements.

Although the PENCIL CODE is mainly designed to run on supercomputers, more than

50% of the users run their code also on Macs, and the other half uses either directly

Linux on their laptops or they use VirtualBox on their Windows machine on which they

install Ubuntu Linux. If you have

IDL

as well, you will be able to visualize the re-

sults (a number of sample procedures are provided), but other tools such as

Python

(OpenDX, data explorer) can also be used and some relevant tools and routines come

with the PENCIL CODE.

If you want to make creative use of the code, this manual will contain far too little in-

formation. Its major aim is to give you an idea of the way the code is organized, so you

can more efﬁciently read the source code, which contains a reasonable amount of com-

ments. You might want to read through the various sample directories that are checked

in. Choose one that is closest to your application and start modifying. For further en-

hancements that you may want to add to the code, you can take as an example the lines

in the code that deal with related variables, functions, diagnostics, equations etc., which

have already been implemented. Just remember: grep is one of your best friends when

you want to understand how certain variables or functions are used in the code.

We will be happy to include user-supplied changes and updates to the code in future

releases and welcome any feedback.

wdobler@gmail.com Potsdam

AxelBrandenburg@gmail.com Stockholm

viii

Acknowledgments

Many people have contributed in different ways to the development of this code. We

thank ﬁrst of all ˚

Ake Nordlund (Copenhagen Observatory) and Bob Stein (University of

Michigan) who introduced us to the idea of using high-order schemes in compressible

ﬂows and who taught us a lot about simulations in general.

The calculation of the power spectra, structure functions, the remeshing procedures,

routines for changing the number of processors, as well as the shearing sheet approxi-

mation and the ﬂux-limited diffusion approximation for radiative transfer were imple-

mented by Nils Erland L. Haugen (University of Trondheim). Tobi Heinemann added

the long characteristics method for radiative transfer as well as hydrogen ionization.

He also added and/or improved shock diffusion for other variables and improved the

resulting timestep control. Anders Johansen, Wladimir (Wlad) Lyra, and Jeff Oishi con-

tributed to the implementation of the dust equations (which now comprises an array of

different components). Antony (Tony) Mee (University of Newcastle) implemented shock

viscosity and added the interstellar module together with Graeme R. Sarson (also Uni-

versity of Newcastle), who also implemented the geodynamo set-up together with David

McMillan (currently also at the University of Newcastle). Tony also included a method

for outputting auxiliary variables and enhanced the overall functionality of the code

and related idl and dx procedures. He also added, together with Andrew Snodin, the

evolution equations for the cosmic ray energy density. Vladimir Pariev (University of

Rochester) contributed to the development and testing of the potential ﬁeld boundary

condition at an early stage. The implementation of spherical and cylindrical coordinates

is due to Dhrubaditya (Dhruba) Mitra and Wladimir Lyra. Wlad also implemented the

global set-up for protoplanetary disks (as opposed to the local shearing sheet formalism).

He also added a N-body code (based on the particle module coded by Anders Johansen

and Tony), and implemented the coupled evolution equations of neutrals and ions for

two-ﬂuid models of ambipolar diffusion. Boris Dintrans is in charge of implementing the

anelastic and Boussinesq modules. Philippe-A. Bourdin implemented HDF5 support and

wrote the optional IO-modules for high-performance computing featuring various com-

munication strategies. He also contributed to the solar-corona module and worked on

the IDL GUI, including the IDL routines for reading and working with large amounts of

data. Again, this list contains other recent items that are not yet fully documented and

acknowledged.

Use of the PPARC supported supercomputers in St Andrews (Mhd) and Leicester (Ukaff)

is acknowledged. We also acknowledge the Danish Center for Scientiﬁc Computing for

granting time on Horseshoe, which is a 512+140 processor Beowulf cluster in Odense

(Horseshoe).

Contents

I Using the PENCIL CODE 1

1 System requirements 1

2 Obtaining the code 2

2.1 Obtaining the code via git or svn . . . . . . . . . . . . . . . . . . . . . . . . 2

2.2 Updating via svn or git . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

2.3 Getting the last validated version . . . . . . . . . . . . . . . . . . . . . . . . 3

2.4 Getting older versions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4

3 Getting started 5

3.1 Setup . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 5

3.1.1 Environment settings . . . . . . . . . . . . . . . . . . . . . . . . . . . 5

3.1.2 Linking scripts and source ﬁles . . . . . . . . . . . . . . . . . . . . . 6

3.1.3 Adapting ‘Makefile.src’ ......................... 6

3.1.4 Running make ............................... 6

3.1.5 Choosing a data directory . . . . . . . . . . . . . . . . . . . . . . . . 7

3.1.6 Running the code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7

3.2 Further tests . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

4 Code structure 11

4.1 Directory tree . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

4.2 Basic concepts . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12

4.2.1 Data access in pencils . . . . . . . . . . . . . . . . . . . . . . . . . . 12

4.2.2 Modularity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13

4.3 Files in the run directories . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14

4.3.1 ‘start.in’, ‘run.in’, ‘print.in’ . . . . . . . . . . . . . . . . . . . . . . 14

4.3.2 ‘datadir.in’ ................................ 14

4.3.3 ‘reference.out’ .............................. 14

4.3.4 ‘start.csh’, ‘run.csh’, ‘getconf.csh’ [obsolete; see Sect. 5.1] . . . . . 14

4.3.5 ‘src/ ’.................................... 14

4.3.6 ‘data/ ’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15

5 Using the code 17

5.1 Conﬁguring the code to compile and run on your computer . . . . . . . . . 17

5.1.1 Locating the conﬁguration ﬁle . . . . . . . . . . . . . . . . . . . . . . 17

5.1.2 Structure of conﬁguration ﬁles . . . . . . . . . . . . . . . . . . . . . 18

5.1.3 Compiling the code . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

5.1.4 Running the code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

5.1.5 Testing the code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 20

5.2 Adapting ‘Makefile.src’ [obsolete; see Sect. 5.1] . . . . . . . . . . . . . . . 21

5.3 Changing the resolution . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 22

5.4 Using a non-equidistant grid . . . . . . . . . . . . . . . . . . . . . . . . . . 23

5.5 Diagnostic output . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25

5.6 Data ﬁles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25

5.6.1 Snapshot ﬁles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 25

5.7 Video ﬁles and slices . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 26

5.8 Averages . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29

5.8.1 One-dimensional output averaged in two dimensions . . . . . . . . 29

5.8.2 Two-dimensional output averaged in one dimension . . . . . . . . . 29

5.8.3 Azimuthal averages . . . . . . . . . . . . . . . . . . . . . . . . . . . . 29

5.8.4 Time averages . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 30

5.9 Helper scripts . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 31

5.10 RELOAD and STOP ﬁles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 33

5.11 RERUN and NEWDIR ﬁles . . . . . . . . . . . . . . . . . . . . . . . . . . . 34

5.12 Start and run parameters . . . . . . . . . . . . . . . . . . . . . . . . . . . . 34

5.13 Physical units . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 36

5.14 Minimum amount of viscosity . . . . . . . . . . . . . . . . . . . . . . . . . . 37

5.15 The time step . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 38

5.15.1 The usual RK-2N time step . . . . . . . . . . . . . . . . . . . . . . . 38

5.15.2 The Runge-Kutta-Fehlberg time step . . . . . . . . . . . . . . . . . . 38

5.16 Boundary conditions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39

5.16.1 Where to specify boundary conditions . . . . . . . . . . . . . . . . . 39

5.16.2 How to specify boundary conditions . . . . . . . . . . . . . . . . . . 39

5.17 Restarting a simulation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 40

5.18 One- and two-dimensional runs . . . . . . . . . . . . . . . . . . . . . . . . . 41

5.19 Visualization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41

5.19.1 Gnuplot . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41

5.19.2 Data explorer . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41

5.19.3 GDL . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 42

5.19.4 IDL . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 43

5.19.5 Python . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46

5.20 Running on multi-processor computers . . . . . . . . . . . . . . . . . . . . . 49

5.20.1 How to run a sample problem in parallel . . . . . . . . . . . . . . . 49

5.20.2 Hierarchical networks (e.g. on Beowulf clusters) . . . . . . . . . . . 50

5.20.3 Extra workload caused by the ghost zones . . . . . . . . . . . . . . . 50

5.21 Running in double-precision . . . . . . . . . . . . . . . . . . . . . . . . . . . 51

5.22 Power spectrum . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 52

5.23 Structure functions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 54

5.24 Particles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55

5.24.1 Particles in parallel . . . . . . . . . . . . . . . . . . . . . . . . . . . . 56

5.24.2 Large number of particles . . . . . . . . . . . . . . . . . . . . . . . . 58

5.24.3 Random number generator . . . . . . . . . . . . . . . . . . . . . . . 58

5.25 Non-cartesian coordinate systems . . . . . . . . . . . . . . . . . . . . . . . . 59

6 The equations 60

6.1 Continuity equation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 60

6.2 Equation of motion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 60

6.3 Induction equation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 61

6.4 Entropy equation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 61

6.4.1 Viscous heating . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62

6.4.2 Alternative description . . . . . . . . . . . . . . . . . . . . . . . . . . 62

6.5 Transport equation for a passive scalar . . . . . . . . . . . . . . . . . . . . 63

6.6 Bulk viscosity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 63

6.6.1 Shock viscosity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 63

6.7 Equation of state . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 63

6.8 Ionization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 64

6.8.1 Ambipolar diffusion . . . . . . . . . . . . . . . . . . . . . . . . . . . . 65

6.9 Combustion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

6.10 Radiative transfer . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

6.11 Self-gravity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 67

6.12 Incompressible and anelastic equations . . . . . . . . . . . . . . . . . . . . 67

6.13 Dust equations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 68

6.14 Cosmic ray pressure in diffusion approximation . . . . . . . . . . . . . . . 69

6.15 Chiral MHD . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 69

6.16 Particles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 70

6.16.1 Tracer particles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71

6.16.2 Dust particles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71

6.17 N-body solver . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72

6.18 Test-ﬁeld equations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 73

6.19 Gravitational wave equations . . . . . . . . . . . . . . . . . . . . . . . . . . 73

7 Troubleshooting / Frequently Asked Questions 76

7.1 Download and setup . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 76

7.1.1 Download forbidden . . . . . . . . . . . . . . . . . . . . . . . . . . . . 76

7.1.2 Shell gives error message when sourcing ‘sourceme.X’ . . . . . . . . 76

7.2 Compilation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 77

7.2.1 Problems compiling syscalls . . . . . . . . . . . . . . . . . . . . . . . 77

7.2.2 Unable to open include ﬁle: chemistry.h . . . . . . . . . . . . . . . . 77

7.2.3 Compiling with

ifc

under Linux . . . . . . . . . . . . . . . . . . . . . 77

7.2.4 Segmentation fault with

ifort

8.0 under Linux . . . . . . . . . . . . 78

7.2.5 The underscore problem: linking with

MPI

. . . . . . . . . . . . . . 78

7.2.6 Compilation stops with the cryptic error message: . . . . . . . . . . 78

7.2.7 The code doesn’t compile, . . . . . . . . . . . . . . . . . . . . . . . . . 79

7.2.8 Some samples don’t even compile, . . . . . . . . . . . . . . . . . . . 79

7.2.9 Internal compiler error with Compaq/Dec F90 . . . . . . . . . . . . 80

7.2.10 Assertion failure under SunOS . . . . . . . . . . . . . . . . . . . . . 80

7.2.11 After some dirty tricks I got pencil code to compile with MPI, ... . . 81

7.2.12 Error: Symbol ’mpi comm world’ at (1) has no IMPLICIT type . . . 81

7.2.13 Error: Can’t open included ﬁle ’mpif.h’ . . . . . . . . . . . . . . . . . 82

7.3 Pencil check . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 82

7.3.1 The pencil check complains for no reason. . . . . . . . . . . . . . . . 82

7.3.2 The pencil check reports MISSING PENCILS and quits . . . . . . 82

7.3.3 The pencil check reports unnecessary pencils . . . . . . . . . . . . . 82

7.3.4 The pencil check reports that most or all pencils are missing . . . . 82

7.3.5 Running the pencil check triggers mathematical errors in the code 83

7.3.6 The pencil check still complains . . . . . . . . . . . . . . . . . . . . . 83

7.3.7 The pencil check is annoying so I turned it off . . . . . . . . . . . . 83

7.4 Running . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 83

7.4.1 Periodic boundary conditions in ‘start.x’ . . . . . . . . . . . . . . . 83

7.4.2 csh problem? . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 83

7.4.3 ‘run.csh’ doesn’t work: . . . . . . . . . . . . . . . . . . . . . . . . . . 84

7.4.4 Code crashes after restarting . . . . . . . . . . . . . . . . . . . . . . 84

7.4.5 auto-test gone mad...? . . . . . . . . . . . . . . . . . . . . . . . . . . 84

7.4.6 Can I restart with a different number of cpus? . . . . . . . . . . . . 85

7.4.7 Can I restart with a different number of cpus? . . . . . . . . . . . . 85

7.4.8 fft xyz parallel 3D: nygrid needs to be an integer multiple... . . . . 85

xii

7.4.9 Unit-agnostic calculations? . . . . . . . . . . . . . . . . . . . . . . . 86

7.5 Visualization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 87

7.5.1 ‘start.pro’ doesn’t work: . . . . . . . . . . . . . . . . . . . . . . . . . 87

7.5.2 ‘start.pro’ doesn’t work: . . . . . . . . . . . . . . . . . . . . . . . . . 87

7.5.3 Something about tag name undeﬁned: . . . . . . . . . . . . . . . . . 87

7.5.4 Something INC in start.pro . . . . . . . . . . . . . . . . . . . . . . . 87

7.5.5 nl2idl problem when reading param2.nml . . . . . . . . . . . . . . . 88

7.5.6 Spurious dots in the time series ﬁle . . . . . . . . . . . . . . . . . . 88

7.5.7 Problems with pc_varcontent.pro . . . . . . . . . . . . . . . . . . . 88

7.6 General questions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 89

7.6.1 “Installation” procedure . . . . . . . . . . . . . . . . . . . . . . . . . 89

7.6.2 Small numbers in the code . . . . . . . . . . . . . . . . . . . . . . . . 89

7.6.3 Why do we need a /lphysics/ namelist in the ﬁrst place? . . . . . . 90

7.6.4 Can I run the code on a Mac? . . . . . . . . . . . . . . . . . . . . . . 91

7.6.5 Pencil Code discussion forum . . . . . . . . . . . . . . . . . . . . . . 91

7.6.6 The manual . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 91

II Programming the PENCIL CODE 93

8 Understanding the code 97

8.1 Example: how is the continuity equation being solved? . . . . . . . . . . . 97

9 Adapting the code 99

9.1 The PENCIL CODE coding standard . . . . . . . . . . . . . . . . . . . . . . . 99

9.2 Adding new output diagnostics . . . . . . . . . . . . . . . . . . . . . . . . . 100

9.3 The f-array . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 102

9.4 The df-array . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 102

9.5 The fp-array . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 103

9.6 The pencil case . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 103

9.6.1 Pencil check . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104

9.6.2 Adding new pencils . . . . . . . . . . . . . . . . . . . . . . . . . . . . 105

9.7 Adding new physics: the Special module . . . . . . . . . . . . . . . . . . . . 105

9.8 Adding switchable modules . . . . . . . . . . . . . . . . . . . . . . . . . . . 106

9.9 Adding your initial conditions: the InitialCondition module . . . . . . . . . 106

10 Testing the code 108

10.1 How to set up periodic tests (auto-tests) . . . . . . . . . . . . . . . . . . . . 108

11 Useful internals 110

11.1 Global variables . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 110

11.2 Subroutines and functions . . . . . . . . . . . . . . . . . . . . . . . . . . . . 110

III Appendix 113

A Timings 113

A.1 Test case . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 120

A.2 Running the code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 121

A.3 Triolith . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 121

A.4 Lindgren . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 121

xiii

B Coding standard 124

B.1 File naming conventions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 124

B.2 Fortran Code . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 124

B.2.1 Indenting and whitespace . . . . . . . . . . . . . . . . . . . . . . . . 124

B.2.2 Comments . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 125

B.2.3 Module names . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 126

B.2.4 Variable names . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 126

B.2.5 Emacs settings . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 127

B.3 Other best practices . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 128

B.4 General changes to the code . . . . . . . . . . . . . . . . . . . . . . . . . . . 128

C Some speciﬁc initial conditions 129

C.1 Random velocity or magnetic ﬁelds . . . . . . . . . . . . . . . . . . . . . . . 129

C.2 Turbulent initial with given spectrum . . . . . . . . . . . . . . . . . . . . . 129

C.3 Beltrami ﬁelds . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 130

C.4 Magnetic ﬂux rings: initaa=’fluxrings’ . . . . . . . . . . . . . . . . . . . 130

C.5 Vertical stratiﬁcation . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 131

C.5.1 Isothermal atmosphere . . . . . . . . . . . . . . . . . . . . . . . . . . 131

C.5.2 Polytropic atmosphere . . . . . . . . . . . . . . . . . . . . . . . . . . 132

C.5.3 Changing the stratiﬁcation . . . . . . . . . . . . . . . . . . . . . . . 133

C.5.4 The Rayleigh number . . . . . . . . . . . . . . . . . . . . . . . . . . . 133

C.5.5 Entropy boundary condition . . . . . . . . . . . . . . . . . . . . . . . 134

C.5.6 Temperature boundary condition at the top . . . . . . . . . . . . . . 134

C.6 Potential-ﬁeld boundary condition . . . . . . . . . . . . . . . . . . . . . . . 134

C.7 Planet solution in the shearing box . . . . . . . . . . . . . . . . . . . . . . . 136

D Some speciﬁc boundary conditions 137

D.1 Perfect-conductor boundary condition . . . . . . . . . . . . . . . . . . . . . 137

D.2 Stress-free boundary condition . . . . . . . . . . . . . . . . . . . . . . . . . 137

D.3 Normal-ﬁeld-radial boundary condition . . . . . . . . . . . . . . . . . . . . 138

E High-frequency ﬁlters 139

E.1 Conservative hyperdissipation . . . . . . . . . . . . . . . . . . . . . . . . . . 139

E.2 Hyperviscosity . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 141

E.2.1 Conservative case . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 141

E.2.2 Non-conservative cases . . . . . . . . . . . . . . . . . . . . . . . . . . 142

E.2.3 Choosing the coefﬁcient . . . . . . . . . . . . . . . . . . . . . . . . . 143

E.2.4 Turbulence with hyperviscosity . . . . . . . . . . . . . . . . . . . . . 143

E.3 Anisotropic hyperdissipation . . . . . . . . . . . . . . . . . . . . . . . . . . . 144

E.4 Hyperviscosity in Burgers shock . . . . . . . . . . . . . . . . . . . . . . . . 144

F Special techniques 146

F.1 After changing

REAL PRECISION

. . . . . . . . . . . . . . . . . . . . . . . 146

F.2 Remeshing (regridding) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 146

F.3 Restarting from a run with less physics . . . . . . . . . . . . . . . . . . . . 147

F.4 Restarting with particles from a run without them . . . . . . . . . . . . . . 148

G Runs and reference data 150

G.1 Shock tests . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 150

G.1.1 Sod shock tube problem . . . . . . . . . . . . . . . . . . . . . . . . . 150

G.1.2 Temperature jump . . . . . . . . . . . . . . . . . . . . . . . . . . . . 150

xiv

G.2 Random forcing function . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 150

G.3 Three-layered convection model . . . . . . . . . . . . . . . . . . . . . . . . . 151

G.4 Magnetic helicity in the shearing sheet . . . . . . . . . . . . . . . . . . . . 152

H Numerical methods 156

H.1 Sixth-order spatial derivatives . . . . . . . . . . . . . . . . . . . . . . . . . 156

H.2 Upwind derivatives to avoid ‘wiggles’ . . . . . . . . . . . . . . . . . . . . . . 157

H.3 The bidiagonal scheme for cross-derivatives . . . . . . . . . . . . . . . . . . 158

H.4 The 2N-scheme for time-stepping . . . . . . . . . . . . . . . . . . . . . . . . 159

H.5 Diffusive error from the time-stepping . . . . . . . . . . . . . . . . . . . . . 160

H.6 Ionization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 161

H.7 Radiative transfer . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 162

H.7.1 Solving the radiative transfer equation . . . . . . . . . . . . . . . . 162

H.7.2 Angular integration . . . . . . . . . . . . . . . . . . . . . . . . . . . . 163

I Curvilinear coordinates 165

I.1 Covariant derivatives . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165

I.2 Differential operators . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165

I.2.1 Gradient . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165

I.2.2 Divergence . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 166

I.2.3 Curl . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 166

I.2.4 Advection operator . . . . . . . . . . . . . . . . . . . . . . . . . . . . 167

I.2.5 Mixed advection operator . . . . . . . . . . . . . . . . . . . . . . . . 167

I.2.6 Shear term . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 168

I.2.7 Another mixed advection operator . . . . . . . . . . . . . . . . . . . 168

I.2.8 Strain Matrix . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 168

I.2.9 Lambda effect . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 168

I.2.10 Laplacian of a scalar . . . . . . . . . . . . . . . . . . . . . . . . . . . 169

I.2.11 Hessian of a scalar . . . . . . . . . . . . . . . . . . . . . . . . . . . . 169

I.2.12 Double curl . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 170

I.2.13 Gradient of a divergence . . . . . . . . . . . . . . . . . . . . . . . . . 171

J Switchable modules 173

K Startup and run-time parameters 174

K.1 Startup parameters for ‘start.in’ . . . . . . . . . . . . . . . . . . . . . . . . 174

K.2 Runtime parameters for ‘run.in’ . . . . . . . . . . . . . . . . . . . . . . . . 181

K.3 Parameters for ‘print.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 188

K.4 Parameters for ‘video.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 227

K.5 Parameters for ‘phiaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . 228

K.6 Parameters for ‘xyaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . 229

K.7 Parameters for ‘xzaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . 235

K.8 Parameters for ‘yzaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . 237

K.9 Parameters for ‘yaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 239

K.10 Parameters for ‘zaver.in’ . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 241

K.11 Boundary conditions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 244

K.11.1 Boundary condition

bcx

. . . . . . . . . . . . . . . . . . . . . . . . . 244

K.11.2 Boundary condition

bcy

. . . . . . . . . . . . . . . . . . . . . . . . . 247

K.11.3 Boundary condition

bcz

. . . . . . . . . . . . . . . . . . . . . . . . . 249

K.12 Initial condition parameter dependence . . . . . . . . . . . . . . . . . . . . 253

IV Indexes 259

xvi

Part I

Using the PENCIL CODE

1 System requirements

To use the code, you will need the following:

1. Absolutely needed:

•

F95

compiler

•

compiler

2. Used heavily (if you don’t have one of these, you will need to adjust many things

manually):

•a

Unix

Linux

-type system with

make

and

csh

•

Perl

(remember: if it doesn’t run Perl, it’s not a computer)

3. The following are dispensable, but enhance functionality in one way or the other:

•an

MPI

implementation (for parallelization on multiprocessor systems)

•

alias

OpenDX

data explorer

(for 3-D visualization of results)

•

IDL

(for visualization of results; the 7-minute demo license will do for many

applications)

2 THE PENCIL CODE

2 Obtaining the code

The code is now distributed via https://github.com/pencil-code/pencil-code, where

you can either download a tarball, or, preferably, download it via

svn

git

. In Iran and

some other countries, GitHub is not currently available. To alleviate this problem, we

have made a recent copy available on http://www.nordita.org/software/pencil-code/.

If you want us to update this tarball, please contact us.

To ensure at least some level of stability of the

svn/git

versions, a set of test problems

(listed in ‘$PENCIL_HOME/bin/auto-test’) are routinely tested. This includes all problems

in ‘$PENCIL_HOME/samples’. See Sect. 10 for details.

2.1 Obtaining the code via git or svn

1. Many machines have

svn

installed (try svn -v or which svn). On Ubuntu, for ex-

ample,

svn

comes under the package name subversion.

2. The code is now saved under Github, git can be obtained in Linux by typing sudo

apt-get install git

3. Unless you are a privileged users with write access, you can download the code

with the command

git clone https://github.com/pencil-code/pencil-code.git

svn checkout https://github.com/pencil-code/pencil-code/trunk/ ...\\

pencil-code --username MY_GITHUB_USERNAME

In order to push your changes to the repository, you have to ask the maintainer of

pencil code for push access (to become a contributor), or put a pull request to the

maintainer of the code.

Be sure to run auto-test before you check anything back in again. It can be very

annoying for someone else to ﬁgure out what’s wrong, especially if you are just up

to something else. At the very least, you should do

pc_auto-test --level=0 --no-pencil-check -C

This allows you to run just 2 of the most essential tests starting with all the no-

modules and then most-modules.

2.2 Updating via svn or git

Independent of how you installed the code in the ﬁrst place (from tarball or via

svn/git

you can update your version using

svn/git

. If you have done nontrivial alterations to

your version of the code, you ought to be careful about upgrading: although

svn/git

is an

excellent tool for distributed programming, conﬂicts are quite possible, since many of us

are going to touch many parts of the code while we develop it further. Thus, despite the

2.3 Getting the last validated version 3

fact that the code is under

svn/git

, you should probably back up your important changes

before upgrading.

Here is the upgrading procedure for

git

1. Perform a git update of the tree:

unix> git pull

2. Fix any conﬂicts you encounter and make sure the examples in the directory

‘samples/’ are still working.

Here is the upgrading procedure for

svn

1. Perform a svn update of the tree:

unix> pc_svnup

2. Fix any conﬂicts you encounter and make sure the examples in the directory

‘samples/’ are still working.

If you have made useful changes, please contact one of the (currently) 10 “Contributors”

(listed under https://github.com/pencil-code/pencil-code) who can give you push or

check-in permission. Be sure to have sufﬁcient comments in the code and please follow

our standard coding conventions explained in Section 9.1. There is also a script to check

and ﬁx the most common stylebreaks, pc codingstyle.

2.3 Getting the last validated version

The script pc_svnup accepts arguments -val or -validated, which means that the current

changes on a user’s machine will be merged into the last working version. This way

every user can be sure that any problems with the code must be due to the current

changes done by this user since the last check-in.

Examples:

unix> pc_svnup -src -s -validated

brings all ﬁles in ‘$PENCIL_HOME/src’ to the last validated status, and merges all your

changes into this version. This allows you to work with this, but in order to check in

your changes you have to update everything to the most recent status ﬁrst, i.e.

unix> pc_svnup -src

Your own changes will be merged into this latest version as before.

NOTE: The functionality of the head of the trunk should be preserved at all times. How-

ever, accidents do happen. For the beneﬁt of all other developers, any errors should

be corrected within 1-2 hours. This is the reason why the code comes with a ﬁle

‘pencil-code/license/developers.txt’, which should contain contact details of all de-

velopers. The pc_svnup -val option allows all other people to stay away from any trou-

ble.

4 THE PENCIL CODE

2.4 Getting older versions

You may ﬁnd that the latest

svn

version of the code produces errors. If you have reasons

to believe that this is due to changes introduced on 27 November 2008 (to give an ex-

ample), you can check out the version prior to this by specifying a revision number with

svn update -r #####. One reason why one cannot always reproduce exactly the same

situation too far back in time is connected with the fact that processor architecture and

the compiler were different, resulting e.g. in different rounding errors.

3. Getting started 5

3 Getting started

To get yourself started, you should run one or several examples which are provided in

one of the ‘samples/’ subdirectories. Note that you will only be able to fully assess the

numerical solutions if you visualize them with

IDL

or other tools (see Sect. 5.19).

3.1 Setup

3.1.1 Environment settings

The functionality of helper scripts and IDL routines relies on a few environment vari-

ables being set correctly. The simplest way to achieve this is to go to the top directory of

the code and source one of the two scripts ‘sourceme.csh’ or ‘sourceme.sh’ (depending on

the type of shell you are using):

csh> cd pencil-code

csh> source ./sourceme.csh

for

tcsh

csh

users; or

sh> cd pencil-code

sh> . ./sourceme.sh

for users of

bash

Bourne shell

, or similar shells. You should get output similar to

PENCIL_HOME = </home/dobler/f90/pencil-code>

Adding /home/dobler/f90/pencil-code/bin to PATH

Apart from the PATH variable, the environment variable IDL_PATH is set to something

like ./idl:../idl:+$PENCIL_HOME/idl:./data:<IDL_DEFAULT> .

Note 1 The <IDL_DEFAULT> mechanism does not work for IDL versions 5.2 or older. In

this case, you will have to edit the path manually, or adapt the ‘sourceme’ scripts.

Note 2 If you don’t want to rely on the ‘sourceme’ scripts’ (quite heuristic) ability to cor-

rectly identify the code’s main directory, you can set the environment variable PENCIL_-

HOME explicitly before you run the source command.

Note 3 Do not just source the ‘sourceme’ script from your shell startup ﬁle (‘~/.cshrc’

or ‘~/.bashrc’, because it outputs a few lines of diagnostics for each sub-shell, which will

break many applications. To suppress all output, follow the instructions given in the

header documentation of ‘sourceme.csh’ and ‘sourceme.sh’. Likewise, output from other

ﬁles invoked by source should also be suppressed.

Note 4 The second time you source ‘sourceme’, it will not add anything to your PATH

variable. This is on purpose to avoid cluttering of your environment: you can source the

ﬁle as often as you like (in your shell startup script, then manually and in addition in

some script you have written), without thinking twice. If, however, at the ﬁrst sourcing,

the setting of PENCIL_HOME was wrong, this mechanism would keep you from ever adding

6 THE PENCIL CODE

the right directory to your PATH. In this case, you need to ﬁrst undeﬁne the environment

variable PENCIL_HOME:

csh> unsetenv PENCIL_HOME

csh> source ./sourceme.csh

sh> unset PENCIL_HOME

sh> . ./sourceme.sh

3.1.2 Linking scripts and source ﬁles

With your environment set up correctly, you can now go to the directory you want to

work in and set up subdirectories and links. This is accomplished by the script ‘pc_-

setupsrc’, which is located in ‘$PENCIL_HOME/bin’ and is thus now in your executable

path.

For concreteness, let us assume you want to use ‘samples/conv-slab’ as your

run direc-

tory

, i.e. you want to run a three-layer slab model of solar convection. You then do the

following:

unix> cd samples/conv-slab

unix> pc_setupsrc

src already exists

2 files already exist in src

The script has linked a number of scripts from ‘$PENCIL_HOME/bin’, generated a directory

‘src’ for the source code and linked the Fortran source ﬁles (plus a few more ﬁles) from

‘$PENCIL_HOME/src’ to that directory:

unix> ls -F

reference.out src/

start.csh@ run.csh@ getconf.csh@

start.in run.in print.in

3.1.3 Adapting ‘Makefile.src’

This step requires some input from you, but you only have to do this once for each

machine you want to run the code on. See Sect. 5.2 for a description of the steps you

need to take here.

Note: If you are lucky and use compilers similar to the ones we have, you may be able

to skip this step; but blame yourself if things don’t compile, then. If not, you can run

make with explicit ﬂags, see Sect. 5.2 and in particular Table 1.

3.1.4 Running make

Next, you run make in the ‘src’ subdirectory of your run directory. Since you are

using one of the predeﬁned test problems, the settings in ‘src/Makefile.local’ and

‘src/cparam.local’ are all reasonable, and you just do

3.1 Setup 7

unix> make

If you have set up the compiler ﬂags correctly, compilation should complete successfully.

3.1.5 Choosing a data directory

The code will by default write data like snapshot ﬁles to the subdirectory ‘data’ of the

run directory. Since this will involve a large volume of IO-operations (at least for large

grid sizes), one will normally try to avoid writing the data via NFS. The recommended

way to set up a ‘data’ data directory is to generate a corresponding directory on the local

disc of the computer you are running on and (soft-)link it to ‘./data’. Even if the link is

part of an NFS directory, all the IO operations will be local. For example, if you have a

local disc ‘/scratch’, you can do the following:

unix> mkdir -p /scratch/$USER/pencil-data/samples/conv-slab

unix> ln -s /scratch/$USER/pencil-data/samples/conv-slab ./data

This is done automatically by the pc_mkdatadir command which, in turn, is invoked

when making a new run directory with the pc_newrun command, for example.

Even if you don’t have an NFS-mounted directory (say, on your notebook computer), it

is probably still a good idea to have code and data well separated by a scheme like the

one described above.

An alternative to symbolic links, is to provide a ﬁle called ‘datadir.in’ in the root of

the run directory. This ﬁle should contain one line of text specifying the absolute or

relative data directory path to use. This facility is useful if one wishes to switch one run

directory between different data directories. It is suggested that in such cases symbolic

links are again made in the run directory to the various locations, then the ‘datadir.in’

need contain only a short relative path.

3.1.6 Running the code

You are now ready to start the code:

unix> start.csh

Linux cincinnatus 2.4.18-4GB #1 Wed Mar 27 13:57:05 UTC 2002 i686 unknown

Non-MPI version

datadir = data

Fri Aug 8 21:36:43 CEST 2003

src/start.x

CVS: io_dist.f90 v. 1.61 (brandenb ) 2003/08/03 09:26:55

[. . . ]

CVS: start.in v. 1.4 (dobler ) 2002/10/02 20:11:14

nxgrid,nygrid,nzgrid= 32 32 32

thermodynamics: assume cp=1

uu: up-down

piecewise polytropic vertical stratification (lnrho)

init_lnrho: cs2bot,cs2top= 1.450000 0.3333330

e.g. for ionization runs: cs2bot,cs2top not yet set

piecewise polytropic vertical stratification (ss)

8 THE PENCIL CODE

start.x has completed successfully

0.070u 0.020s 0:00.14 64.2% 0+0k 0+0io 180pf+0w

Fri Aug 8 21:36:43 CEST 2003

This runs ‘src/start.x’ to construct an initial condition based on the parameters

set in ‘start.in’. This initial condition is stored in ‘data/proc0/var.dat’ (and in

‘data/proc1/var.dat’, etc. if you run the multiprocessor version). It is fair to say that

this is now a rather primitive routine; see ‘pencil-code/idl/read’ for various reading

routines. You can then visualize the data using standard idl language.

If you visualize the proﬁles using

IDL

(see below), the result should bear some resem-

blance to Fig. 2, but with different values in the ghost zones (the correct values are set

at run-time only) and a simpler velocity proﬁle.

Now we run the code:

unix> run.csh

This executes ‘src/run.x’ and carries out

time steps, where

and other run-time

parameters are speciﬁed in ‘run.in’. On a decent PC (1.7 GHz), 50 time steps take about

10 seconds.

The relevant part of the code’s output looks like

--it----t-------dt-------urms----umax----rhom------ssm-----dtc----dtu---dtnu---dtchi-

0 0.34 6.792E-03 0.0060 0.0452 14.4708 -0.4478 0.978 0.013 0.207 0.346

10 0.41 6.787E-03 0.0062 0.0440 14.4707 -0.4480 0.978 0.013 0.207 0.345

20 0.48 6.781E-03 0.0064 0.0429 14.4705 -0.4481 0.977 0.012 0.207 0.345

30 0.54 6.777E-03 0.0067 0.0408 14.4703 -0.4482 0.977 0.012 0.207 0.345

40 0.61 6.776E-03 0.0069 0.0381 14.4702 -0.4482 0.977 0.011 0.207 0.346

and lists

1. the number

of the current time step;

2. the time,

;

3. the time step,

;

4. the rms velocity,

urms

=phu2i;

5. the maximum velocity,

umax

= max |u|;

6. the mean density,

rhom

=hρi;

7. the mean entropy,

ssm

=hsi/cp;

8. the time step in units of the acoustic Courant step,

dtc

=δt cs0/δxmin;

9. the time step in units of the advective time step,

dtu

=δt/(cδt δx/ max |u|);

10. the time step in units of viscous time step,

dtnu

=δt/(cδt,vδx2/νmax);

11. the time step in units of the conductive time step,

dtchi

=δt/(cδt,vδx2/χmax).

The entries in this list can be added, removed or reformatted in the ﬁle ‘print.in’, see

Sects 5.5 and K.3. The output is also saved in ‘data/time_series.dat’ and should be

identical to the content of ‘reference.out’.

3.2 Further tests 9

ln ρ

0 1 2 3

−0.5

0.0

0.5

1.0

1.5

−0.02 0.00 0.02 0.04

−0.5

0.0

0.5

1.0

1.5

Entropy s

−0.6−0.4−0.2 0.0 0.2

−0.5

0.0

0.5

1.0

1.5

Temperature T

0.5 1.0 1.5 2.0

−0.5

0.0

0.5

1.0

1.5

Figure 2: Stratiﬁcation of the three-layer convection model in ‘samples/conv-slab’ after 50 timesteps

(t= 0.428). Shown are (from left to right) density ρ, vertical velocity uz, entropy s/cpand temperature

Tas functions of the vertical coordinate zfor about ten different vertical lines in the computational box.

The dashed lines denote domain boundaries: z < −0.68 is the lower ghost zone (points have no physical

signiﬁcance); −0.68 < z < 0is a stably stratiﬁed layer (ds/dz > 0); 0< z < 1is the unstable layer

(ds/dz < 0); 1< z < 1.32 is the isothermal top layer; z > 1.32 is the upper ghost zone (points have no

physical signiﬁcance).

If you have

IDL

, you can visualize the stratiﬁcation with (see Sect. 5.19.4 for details)

unix > idl

IDL > pc_read_var,obj=var,/trimall

IDL > tvscl,var,uu(*,*,0,0)

which shows uxin the xy plane through the ﬁrst meshpoint in the zdirection. There

have been some now outdates speciﬁc routines that produce results like that shown in

Fig. 2.

Note: If you want to run the code with

MPI

, you will probably need to adapt

‘getconf.csh’, which deﬁnes the commands and ﬂags used to run MPI jobs (and which

is sourced by the scripts ‘start.csh’ and ‘run.csh’). Try

csh -v getconf.csh

csh -x getconf.csh

to see how ‘getconf.csh’ makes its decisions. You would add a section for the host name

of your machine with the particular settings. Since ‘getconf.csh’ is linked from the cen-

tral directory ‘pencil-code/bin’, your changes will be useful for all your other runs too.

3.2 Further tests

There is a number of other tests in the ‘samples/’ directory. You can use the script

‘bin/auto-test’ to automatically run these tests and have the output compared to refer-

10 THE PENCIL CODE

ence results.

4. Code structure 11

4 Code structure

4.1 Directory tree

pencil-code

src idl | dx doc bin samples

Makefile conv-slab interlocked-fluxrings ...

srcstart, run

timestep, deriv

equ

hydro | nohydro

density | nodensity

entropy | noentropy

grav_z | grav_r | nograv

magnetic | nomagnetic

Makefile.local

cparam.local

Figure 3: The basic structure of the code

The overall directory structure of the code is shown in Fig. 3. Under ‘pencil-code’, there

are currently the following ﬁles and directories:

bin/ config/ doc/ idl/ license/ perl/ samples/ sourceme.sh utils/

bugs/ dx/ lib/ misc/ README sourceme.csh src/ www/

Almost all of the source code is contained in the directory ‘src/’, but in order to encap-

sulate individual applications, the code is compiled separately for each run in a local

directory ‘src’ below the individual run directory, like e. g. ‘samples/conv-slab/src’.

It may be a good idea to keep your own runs also under

svn

cvs

(which is older than

but similar to

svn

), but this would normally be a different repository. On the machine

where you are running the code, you may want to check them out into a subdirectory of

12 THE PENCIL CODE

‘pencil-code/’. For example, we have our own runs in a repository called ‘pencil-runs’,

so we do

unix> cd $PENCIL_HOME

unix> svn co runs pencil-runs

In this case, ‘runs’ contains individual run directories, grouped in classes (like ‘spher’ for

spherical calculations, or ‘kinematic’ for kinematic dynamo simulations). The current

list of classes in our own ‘pencil-runs’ repository is

1d-tests/ disc/ kinematic/ rings/

2d-tests/ discont/ Misc/ slab_conv/

3d-tests/ discussion/ OLD/ test/

buoy_tube/ forced/ pass_only/

convstar/ interstellar/ radiation/

The directory ‘forced/’ contains some forced turbulence runs (both magnetic and non-

magnetic); ‘gravz/’ contains runs with vertical gravity; ‘rings/’ contains decaying MHD

problems (interlocked ﬂux rings as initial condition, for example); and ‘kinematic/’ con-

tains kinematic dynamo problems where the hydrodynamics is turned off entirely. The

ﬁle ‘samples/README’ should contain an up-to-date list and short description of the indi-

vidual classes.1

The subdirectory ‘src’ of each run directory contains a few local conﬁguration ﬁles (cur-

rently these are ‘Makefile.local’ and ‘cparam.local’) and possibly ‘ctimeavg.local’. To

compile the samples, links the ﬁles ‘.f90’, ‘.c’ and ‘Makefile.src’ need to be linked from

the top ﬁle[src/]src directory to the local directory ‘./src’. These links are set up by the

script pc_setupsrc) when used in the root of a run directory.

General-purpose visualization routines for

IDL

are in the directories ‘idl’ and ‘dx’,

respectively. There are additional and more specialized

IDL

directories in the different

branches under ‘pencil-runs’.

The directory ‘doc’ contains this manual; ‘bin’ contains a number of utility scripts

(mostly written in

csh

and

Perl

), and in particular the ‘start.csh’, ‘run.csh’, and

‘getconf.csh’ scripts. The ‘.svn’ directory is used (you guessed it) by

.svn

, and is not

normally directly accessed by the user; ‘bugs’, ﬁnally is used by us for internal purposes.

The ﬁles ‘sourceme.csh’ and ‘sourceme.sh’ will set up some environment variables — in

particular PATH — and aliases/shell functions for your convenience. If you do not want

to source one of these ﬁles, you need to make sure your

IDL

path is set appropriately

(provided you want to use

IDL

) and you will need to address the scripts from ‘bin’ with

their explicit path name, or adjust your PATH manually.

4.2 Basic concepts

4.2.1 Data access in pencils

Unlike the CRAY computers that dominated supercomputing in the 80s and early 90s,

all modern computers have a cache that constitutes a signiﬁcant bottleneck for many

1Our ‘pencil-runs’ directory also contains runs that were done some time ago. Occasionally, we try to

update these, especially if we have changed names or other input conventions.

4.2 Basic concepts 13

codes. This is the case if large three-dimensional arrays are constantly used within each

time step, which has the obvious advantage of working on long arrays and allows vector-

ization of elementary machine operations. This approach also implies conceptual sim-

plicity of the code and allows extensive use of the intuitive F90 array syntax. However,

a more cache-efﬁcient way of coding is to calculate an entire time step (or substep of a

multi-stage time-stepping scheme) only along a one-dimensional pencil of data within

the numerical grid. This technique is more efﬁcient for modern RISC processors: on

Linux PCs and SGI workstations, for example, we have found a speed-up by about 60%

in some cases. An additional advantage is a drastic reduction in temporary storage for

auxiliary variables within each time step.

4.2.2 Modularity

Each run directory has a ﬁle ‘src/Makefile.local’ in which you choose certain

modules

which tell the code whether or not entropy, magnetic ﬁelds, hydrodynamics, forcing, etc.

should be invoked. For example, the settings for forced turbulent MHD simulations are

HYDRO = hydro

DENSITY = density

ENTROPY = noentropy

MAGNETIC = magnetic

GRAVITY = nogravity

FORCING = forcing

MPICOMM = nompicomm

GLOBAL = noglobal

IO = io_dist

FOURIER = nofourier

This ﬁle will be processed by

make

and the settings are thus assignments of

make

variables. Apart from the physics modules (equation of motion: yes, density [pressure]:

yes, entropy equation: no, magnetic ﬁelds: yes, gravity: no, forcing: yes), a few technical

modules can also be used or deactivated; in the example above, these are

MPI

(switched

off), additional global variables (none), input/output (distributed), and

FFT

(not used).

The table in Sect. J in the Appendix lists all currently available modules.

Note that most of these

make

variables must be set, but they will normally obtain rea-

sonable default values in ‘Makefile’ (so you only need to set the non-standard ones in

‘Makefile.local’). It is by using this switching mechanism through make that we achieve

high ﬂexibility without resorting to excessive amounts of cryptic preprocessor directives

or other switches within the code.

Many possible combinations of modules have already been tested and examples are part

of the distribution, but you may be interested in a combination which was never tried

before and which may not work yet, since the modules are not fully orthogonal. In such

cases, we depend on user feedback for ﬁxing problems and documenting the changes for

others.

2We stress once more that we are not talking about F90 modules here, although there is some connec-

tion, as most of our modules deﬁne F90 modules: For example each of the modules

gravity simple

grav r

and

nogravity

deﬁnes a Fortran module

Gravity

14 THE PENCIL CODE

4.3 Files in the run directories

4.3.1 ‘start.in’, ‘run.in’, ‘print.in’

These ﬁles specify the startup and runtime parameters (see Sects. 5.12 and K.2), and the

list of diagnostic variables to print (see 5.5). They specify the setup of a given simulation

and are kept under

svn

in the individual ‘samples’ directories.

You may want to check for the correctness of these conﬁguration ﬁles by issuing the

command pc_configtest.

4.3.2 ‘datadir.in’

If this ﬁle exists, it must contain the name of an existing directory, which will be used as

data directory

, i. e. the directory where all results are written. If ‘datadir.in’ does not

exist, the data directory is ‘data/’.

4.3.3 ‘reference.out’

If present, ‘reference.out’ contains the output you should obtain in the given run direc-

tory, provided you have not changed any parameters. To see whether the results of your

run are OK, compare ‘time_series.dat’ to ‘reference.out’:

unix> diff data/time_series.dat reference.out

4.3.4 ‘start.csh’, ‘run.csh’, ‘getconf.csh’ [obsolete; see Sect. 5.1]

These are links to ‘$PENCIL_HOME/bin’. You will be constantly using the scripts

‘start.csh’ and ‘run.csh’ to initialize the code. Things that are needed by both (like the

name of the mpirun executable,

MPI

options, or the number of processors) are located in

‘getconf.csh’, which is never directly invoked.

4.3.5 ‘src/ ’

The ‘src’ directory contains two local ﬁles, ‘src/Makefile.local’ and ‘src/cparam.local’,

which allow the user to choose individual modules (see 4.2.2) and to set parameters like

the grid size and the number of processors for each direction. These two ﬁles are part

of the setup of a given simulation and are kept under

svn

in the individual ‘samples’

directories.

The ﬁle ‘src/cparam.inc’ is automatically generated by the script ‘mkcparam’ and contains

the number of fundamental variables for a given setup.

All other ﬁles in ‘src/’ are either links to source ﬁles (and ‘Makefile.src’) in the

‘$PENCIL_HOME/src’ directory, or object and module ﬁles generated by the compiler.

4.3 Files in the run directories 15

4.3.6 ‘data/ ’

This directory (the name of which will actually be overwritten by the ﬁrst line of

‘datadir.in’, if that ﬁle is present; see §4.3.2) contains the output from the code:

‘data/dim.dat’The global array dimensions.

‘data/legend.dat’The header line specifying the names of the diagnostic variables in

‘time_series.dat’.

‘data/time_series.dat’Time series of diagnostic variables (also printed to stdout). You

can use this ﬁle directly for plotting with

Gnuplot

IDL

Xmgrace

or similar tools (see

also §5.19).

‘data/tsnap.dat’, ‘data/tvid.dat’Time when the next snapshot ‘VARN’ or animation

slice should be taken.

‘data/params.log’Keeps a log of all your parameters: ‘start.x’ writes the startup pa-

rameters to this ﬁle, ‘run.x’ appends the runtime parameters and appends them anew,

each time you use the ‘RELOAD’ mechanism (see §5.10).

‘data/param.nml’Complete set of startup parameters, printed as Fortran namelist.

This ﬁle is read in by ‘run.x’ (this is how values of startup parameters are propagated

to ‘run.x’) and by

IDL

(if you use it).

‘data/param2.nml’Complete set of runtime parameters, printed as Fortran namelist.

This ﬁle is read by

IDL

(if you use it).

‘data/index.pro’Can be used as include ﬁle in

IDL

and contains the column in which

certain variables appear in the diagnostics ﬁle (‘time_series.dat’). It also contains the

positions of variables in the ‘VARN’ ﬁles. These positions depend on whether

entropy

noentropy

, etc, are invoked. This is a temporary solution and the ﬁle may disappear in

future releases.

‘data/interstellar.dat’Unformatted ﬁle containing the time at which the next su-

pernova event will occur, under certain supernova schemes. (Only needed by the

inter-

stellar

module.)

‘data/proc0’, ‘data/proc1’, . . . These are the directories containing data from the in-

dividual processors. So after running an

MPI

job on two processors, you will have the

two directories ‘data/proc0’ and ‘data/proc1’. Each of the directories can contain the

following ﬁles:

‘var.dat’binary ﬁle containing the latest snapshot;

16 THE PENCIL CODE

‘VARN’binary ﬁle containing individual snapshot number N;

‘dim.dat’ASCII ﬁle containing the array dimensions as seen by the given processor;

‘time.dat’ASCII ﬁle containing the time corresponding to ‘var.dat’ (not actually used

by the code, unless you use the

io mpiodist.f90

module);

‘grid.dat’binary ﬁle containing the part of the grid seen by the given processor;

‘seed.dat’the random seed for the next time step (saved for reasons of reproducibility).

For multi-processor runs with velocity forcing, the ﬁles ‘procN/seed.dat’ must all

contain the same numbers, because globally coherent waves of given wavenumber

are used;

‘X.xy’, ‘X.xz’, ‘X.yz’two-dimensional sections of variable X, where Xstands for the

corresponding variable. The current list includes

bx.xy bx.xz by.xy by.xz bz.xy bz.xz divu.xy lnrho.xz

ss.xz ux.xy ux.xz uz.xy uz.xz

Each processor writes its own slice, so these need to be reassembled if one wants

to plot a full slice.

5. Using the code 17

5 Using the code

5.1 Conﬁguring the code to compile and run on your computer

Note: We recommend to use the procedure described here, rather than the old method

described in Sects. 5.2 and 4.3.4.

Quick instructions: You may compile with a default compiler-speciﬁc conﬁguration:

1. Single-processor using the GNU compiler collection:

unix> pc_build -f GNU-GCC

2. Multi-processor using GNU with MPI support:

unix> pc_build -f GNU-GCC_MPI

Many compilers are supported already, please refer to the available conﬁg ﬁles in

‘$PENCIL_HOME/config/compilers/*.conf’, e.g. ‘Intel.conf’ and ‘Intel_MPI.conf’.

If you have to set up some compiler options speciﬁc to a certain host system you work on,

or if you like to create a host-speciﬁc conﬁguration ﬁle so that you can simply execute

pc_build without any options, you can clone an existing host-ﬁle, just include an existing

compiler conﬁguration, and simply only add the options you need. A good example of

a host-ﬁle is ‘$PENCIL_HOME/config/hosts/IWF/host-andromeda-GNU_Linux-Linux.conf’.

You may save a clone under ‘$PENCIL_HOME/config/hosts/<ID>.conf’, where ‘<ID>’ is to

be replaced by the output of pc_build -i. This will be the new default for pc_build.

If you don’t know what this was all about, read on.

In essence, conﬁguration, compiling and running the code work like this:

1. Create a conﬁguration ﬁle for your computer’s host ID.

2. Compile the code using pc_build.

3. Run the code using pc_run

In the following, we will discuss the essentials of this scheme. Exhaustive documen-

tation is available with the commands perldoc Pencil::ConfigFinder and perldoc

PENCIL::ConfigParser.

5.1.1 Locating the conﬁguration ﬁle

Commands like pc_build and pc_run use the Perl module ‘Pencil::ConfigFinder’ to lo-

cate an appropriate conﬁguration ﬁle and ‘Pencil::ConfigParser’ to read and interpret

it. When you use ‘ConfigFinder’ on a given computer, it constructs a host ID for the sys-

tem it is running on, and looks for a ﬁle ‘host_ID.conf’ in any subdirectory of ‘$PENCIL_-

HOME/config/hosts’.

E.g., if the host ID is “workhorse.pencil.org”, ‘ConfigFinder’ would consider the ﬁle

‘$PENCIL_HOME/config/hosts/pencil.org/workhorse.pencil.org.conf’.

18 THE PENCIL CODE

Note 1: The location in the tree under ‘hosts/’ is irrelevant, which allows you to group

related hosts by institution, owner, hardware, etc.

Note 2: ‘ConfigFinder’ actually uses the following search path:

1. ‘./config’

2. ‘$PENCIL_HOME/config-local’

3. ‘$HOME/.pencil/config-local’

4. ‘$PENCIL_HOME/config’

This allows you to override part of the ‘config/’ tree globally on the given ﬁle system,

or locally for a particular run directory, or for one given copy of the PENCIL CODE. This

search path is used both, for locating the conﬁguration ﬁle for your host ID, and for

locating included ﬁles (see below).

The host ID is constructed based on information that is easily available for your system.

The algorithm is as follows:

1. Most commands using ‘ConfigFinder’ have a ‘--host-id’ (sometimes abbreviated

as ‘-H’) option to explicitly set the host ID.

2. If the environment variable

PENCIL HOST ID

is set, its value is used.

3. If any of the ﬁles ‘./host-ID’, ‘$PENCIL_HOME/host-ID’, ‘$HOME/.pencil/host-ID’, ex-

ists, its ﬁrst line is used.

4. If ‘ConfigFinder’ can get hold of a

fully qualiﬁed host name

, that is used as host

ID.

5. Else, a combination of host name, operating system name and possibly some other

information characterizing the system is used.

6. If no conﬁg ﬁle for the host ID is found, the current operating system name is tried

as fallback host ID.

To see which host IDs are tried (up to the ﬁrst one for which a conﬁguration ﬁle is found),

run

unix> pc_build --debug-config

This command will tell you the host-ID of the system that you are using:

unix> pc_build -i

5.1.2 Structure of conﬁguration ﬁles

It is strongly recommended to include in a users conﬁguration ﬁle one of the preset

compiler suite conﬁguration ﬁles. Then, only minor options need to be set by a user, e.g.

the optimization ﬂags. One of those user conﬁguration ﬁles looks rather simple:

# Simple config file. Most files don’t need more.

%include compilers/GNU-GCC

or if you prefer a different compiler:

5.1 Conﬁguring the code to compile and run on your computer 19

# Simple Intel compiler suite config file.

%include compilers/Intel

A more complex ﬁle (using MPI with additional options) would look like this:

# More complex config file.

%include compilers/GNU-GCC_MPI

%section Makefile

MAKE_VAR1 = -j4 # joined compilation with four threads

FFLAGS += -O3 -Wall -fbacktrace # don’t redefine, but append with ’+=’

%endsection Makefile

%section runtime

mpiexec = mpirun # some MPI backends need a redefinition of mpiexec

%endsection runtime

%section environment

SCRATCH_DIR=/var/tmp/$USER

%endsection environment

Adding ” MPI” to a compiler suite’s name is usually sufﬁcient to use MPI.

Note 3: We strongly advise not to mix Fortran- and C-compilers from different manu-

facturers or versions by manually including multiple separate compiler conﬁgurations.

Note 4: We strongly advise to use at maximum the optimization levels ’-O2’ for the

Intel compiler and ’-O3’ for all other compilers. Higher optimization levels implicate an

inadequate loss of precision.

The ‘.conf’ ﬁles consist of the following elements:

Comments: A#sign and any text following it on the same line are ignored.

Sections: There are three sections:

Makeﬁle for setting make parameters

runtime for adding compiler ﬂags used by pc_run

environment shell environment variables for compilation and running

Include statements: An %include ... statement is recursively replaced by the con-

tents of the ﬁles it points to.3

The included path gets a .conf sufﬁx appended. Included paths are typically “ab-

solute”, e.g.

%include os/Unix

will include the ﬁle ‘os/Unix.conf’ in the search path listed above (typically from

‘$PENCIL_HOME/config’). However, if the included path starts with a dot, it is a rel-

ative path, so

3However, if the include statement is inside a section, only the ﬁle’s contents inside that section are

inserted.

20 THE PENCIL CODE

%include ./Unix

will only search in the directory where the including ﬁle is located.

Assignments: Statements like FFLAGS += -O3 or mpiexec=mpirun are assignments and

will set parameters that are used by pc_build/make or pc_run.

Lines ending with a backslash ‘\’ are continuation lines.

If possible, one should always use incremental assignments, indicated by using a

+= sign instead of =, instead of redeﬁning certain ﬂags.

Thus,

CFLAGS += -O3

CFLAGS += -I../include -Wall

is the same as

CFLAGS = $(CFLAGS) -O3 -I../include -Wall

5.1.3 Compiling the code

Use the pc_build command to compile the code:

unix> pc_build # use default compiler suite

unix> pc_build -f Intel_MPI # specify a compiler suite

unix> pc_build -f os/GNU_Linux,mpi/open-mpi # explicitly specify config files

unix> pc_build VAR=something # set variables for the makefile

unix> pc_build --cleanall # remove generated files

The third example circumvents the whole host ID mechanism by explicitly instructing

pc_build which conﬁguration ﬁles to use. The fourth example shows how to deﬁne extra

variables (VAR=something) for the execution of the Makefile.

See pc_build --help for a complete list of options.

5.1.4 Running the code

Use the pc_run command to run the code:

unix> pc_run # start if necessary, then run

unix> pc_run start

unix> pc_run run

unix> pc_run start run^3 # start, then run 3 times

unix> pc_run start run run run # start, then run 3 times

unix> pc_run ^3 # start if necessary, then run 3 times

See pc_run --help for a complete list of options.

5.1.5 Testing the code

The pc_auto-test command uses pc_build for compiling and pc_run for running the

tests. Here are a few useful options:

5.2 Adapting ‘Makefile.src’ﬁle]Makeﬁle.src@Makefile.src [obsolete; see Sect. 5.1]21

unix> pc_auto-test

unix> pc_auto-test --no-pencil-check # suppress pencil consistency check

unix> pc_auto-test --max-level=1 # run only tests in level 0 and 1

unix> pc_auto-test --time-limit=2m # kill each test after 2 minutes

See pc_auto-test --help for a complete list of options.

The pencil-test script will use pc_auto-test if given the ‘--use-pc_auto-test’ or ‘-b’

option:

unix> pencil-test --use-pc_auto-test

unix> pencil-test -b # ditto

unix> pencil-test -b -Wa,--max-level=1,--no-pencil-check # quick pencil

See pencil-test --help for a complete list of options.

5.2 Adapting ‘Makefile.src’ [obsolete; see Sect. 5.1]

By default, one should use the above described conﬁguration mechanism for compila-

tion. If for whatever reason one needs to work with a modiﬁed ‘Makefile’, there is a

mechanism for picking the right set of compiler ﬂags based on the hostname.

To give you an idea of how to add your own machines, let us assume you have several

Linux boxes running a compiler f95 that needs the options ‘-O2 -u’, while one of them,

Janus

, runs a compiler f90 which needs the ﬂags ‘-O3’ and requires the additional op-

tions ‘-lmpi -llam’ for

MPI

The ‘Makefile.src’ you need will have the following section:

### Begin machine dependent

## IRIX64:

[. . . ] (leave as it is in the original Makeﬁle)

## OSF1:

[. . . ] (leave as it is in the original Makeﬁle)

## Linux:

[. . . ] (leave everything from original Makeﬁle and add:)

#FC=f95

#FFLAGS=-O2 -u

#FC=f90 #(Janus)

#FFLAGS=-O3 #(Janus)

#LDMPI=-lmpi -llam #(Janus)

## SunOS:

[. . . ] (leave as it is in the original Makeﬁle)

## UNICOS/mk:

[. . . ] (leave as it is in the original Makeﬁle)

## HI-UX/MPP:

[. . . ] (leave as it is in the original Makeﬁle)

## AIX:

[. . . ] (leave as it is in the original Makeﬁle)

22 THE PENCIL CODE

Table 1: Compiler ﬂags for common compilers. Note that some combinations of OS and compiler require

much more elaborate settings; also, if you use MPI, you will have to set LDMPI.

Compiler FC FFLAGS CC CFLAGS

Unix/POSIX:

GNU gfortran -O3 gcc -O3 -DFUNDERSC=1

Intel ifort -O2 icc -O3 -DFUNDERSC=1

PGI pgf95 -O3 pgcc -O3 -DFUNDERSC=1

G95 g95 -O3 -fno-second-underscore gcc -O3 -DFUNDERSC=1

Absoft f95 -O3 -N15 gcc -O3 -DFUNDERSC=1

IBM XL xlf95 -qsuffix=f=f90 -O3 xlc -O3 -DFUNDERSC=1

outdated:

IRIX Mips f90 -64 -O3 -mips4 cc -O3 -64 -DFUNDERSC=1

Compaq f90 -fast -O3 cc -O3 -DFUNDERSC=1

### End machine dependent

Note 1 There is a script for adapting the Makeﬁle: ‘adapt-mkfile’. In the example

above, #(Janus) is not a comment, but marks this line to be activated (uncommented) by

adapt-mkfile if your hostname (‘uname -n‘) matches ‘Janus’ or ‘janus’ (capitalization

is irrelevant). You can combine machine names with a vertical bar: a line containing

#(onsager|Janus) will be activated on both,

Janus

and

Onsager

Note 2 If you want to experiment with compiler ﬂags, or if you want to get things

running without setting up the machine-dependent section of the ‘Makefile’, you can set

make

variables at the command line in the usual manner:

src> make FC=f90 FFLAGS=’-fast -u’

will use the compiler f90 and the ﬂags ‘-fast -u’ for both compilation and linking. Ta-

ble 1 summarizes ﬂags we use for common compilers.

5.3 Changing the resolution

It is advisable to produce a new run directory each time you run a new case. (This does

not include restarts from an old run, of course.) If you have a 323run in some directory

‘runA_32a’, then go to its parent directory, i.e.

runA_32a> cd ..

forced> pc_newrun runA_32a runA_64a

forced> cd runA_64a/src

forced> vi cparam.local

and edit the ‘cparam.local’ for the new resolution.

If you have ever wondered why we don’t do dynamic allocation of the main variable (f)

array, the main reason it that with static allocation the compiler can check whether we

are out of bounds.

5.4 Using a non-equidistant grid 23

5.4 Using a non-equidistant grid

We introduce a non-equidistant grid zi(by now, this is also implemented for the other

directions) as a function z(ζ)of an equidistant grid ζiwith grid spacing ∆ζ= 1.

The way the parameters are handled, the box size and position are not changed when

you switch to a non-equidistant grid, i.e. they are still determined by

xyz0

and

Lxyz

The ﬁrst and second derivatives can be calculated by

dz =df

dζ

dz =1

z′f′(ζ),d2f

dz2=1

z′2f′′(ζ)−z′′

z′3f′(ζ),(1)

which can be written somewhat more compactly using the inverse function ζ(z):

dz =ζ′(z)f′(ζ),d2f

dz2=ζ′2(z)f′′(ζ) + ζ′′(z)ζ′(z)f′(ζ).(2)

Internally, the code uses the quantities

dz 1

≡1/z′=ζ′(z)and

dz tilde

≡ −z′′/z′2=

ζ′′/ζ′, and stores them in ‘data/procN/grid.dat’.

The parameters

lequidist

(a 3-element logical array),

grid func

coeff grid

≥2-element real array) are used to choose a non-equidistant grid and deﬁne

the function z(ζ). So far, one can choose between grid_function=’sinh’,grid_-

function=’linear’ (which produces an equidistant grid for testing purposes), and

grid_function=’step-linear’.

The sinh proﬁle: For grid_function=’sinh’, the function z(ζ)is given by

z(ζ) = z0+Lz

sinh a(ζ−ζ∗) + sinh a(ζ∗−ζ1)

sinh a(ζ2−ζ∗) + sinh a(ζ∗−ζ1),(3)

where z0and z0+Lzare the lowest and uppermost levels, ζ1,ζ2are the ζvalues represent-

ing those levels (normally ζ1= 0, ζ2=Nz−1for a grid of Nzvertical layers [excluding

ghost layers]), and ζ∗is the ζvalue of the inﬂection point of the sinh function. The z

coordinate and ζvalue of the inﬂection point are related via

z∗=z0+Lz

sinh a(ζ∗−ζ1)

sinh a(ζ2−ζ∗) + sinh a(ζ∗−ζ1),(4)

which can be inverted (“after some algebra”) to

ζ∗=ζ1+ζ2

2+1

aartanh 2z∗−z0

Lz−1tanh aζ2−ζ1

2.(5)

General proﬁle: For a general monotonic function ψ() instead of sinh we get,

z(ζ) = z0+Lz

ψ[a(ζ−ζ∗)] + ψ[a(ζ∗−ζ1)]

ψ[a(ζ2−ζ∗)] + ψ[a(ζ∗−ζ1)] ,(6)

and the reference point ζ∗is found by inverting

z∗=z0+Lz

ψ[a(ζ∗−ζ1)]

ψ[a(ζ2−ζ∗)] + ψ[a(ζ∗−ζ1)] ,(7)

numerically.

24 THE PENCIL CODE

Duct ﬂow: The proﬁle function grid_function=’duct’ generates a grid proﬁle for tur-

bulent ﬂow in ducts. For a duct ﬂow, most gradients are steepest close to the walls, and

hence very ﬁne resolution is required near the walls. Here we follow the method of [23]

and use a Chebyshev-type grid with a cosine distribution of the grid points such that in

the ydirection they are located at

yj=hcos θj,(8)

where

θj=(Ny−j)π

Ny−1, j = 1,2,...,Ny(9)

and h=Ly/2is the duct half-width.

Currently this method is only adapted for ducts where xis the stream-wise direction, z

is in the span-wise direction and the walls are at y=y0and y=y0+Ly.

In order to have ﬁne enough resolution, the ﬁrst grid point should be a distance δ=

0.05 lwfrom the wall, where

lw=ν

uτ

, uτ=rτw

ρ,(10)

and τwis the shear wall stress. This is accomplished by using at least

Ny≥N∗

y=π

arccos1−δ

h+ 1 (11)

=πrh

2δ+ 1 −π

24r2δ

h+O"δ

h3/2#(12)

grid points in the y-direction. After rounding up to the next integer value, we ﬁnd that

the truncated condition

Ny≥&πrh

2δ'+ 1 (13)

(where ⌈x⌉denotes the ceiling function, i.e. the smallest integer equal to, or larger than,

x) gives practically identical results.

Example: To apply the sinh proﬁle, you can set the following in ‘start.in’ (this exam-

ple is from ‘samples/sound-spherical-noequi’):

&init_pars

[...]

xyz0 = -2., -2., -2. ! first corner of box

Lxyz = 4., 4., 4. ! box size

lperi = F , F , F ! periodic direction?

lequidist = F, F, T ! non-equidistant grid in z

xyz_star = , , -2. ! position of inflection point

grid_func = , , ’sinh’ ! sinh function: linear for small, but

! exponential for large z

coeff_grid = , , 0.5

5.5 Diagnostic output 25

The parameter array

coeff grid

represents z∗and a; the bottom height z0and the total

box height Lzare taken from

xyz0

and

Lxyz

as in the equidistant case. The inﬂection

point of the sinh proﬁle (the part where it is linear) is not in the middle of the box,

because we have set

xyz star(3)

(i. e. z∗) to −2.

5.5 Diagnostic output

Every

it1

time steps (

it1

is a runtime parameter, see Sect. K.2), the code writes moni-

toring output to

stdout

and, parallel to this, to the ﬁle ‘data/time_series.dat’. The vari-

ables that appear in this listing and the output format are deﬁned in the ﬁle ‘print.in’

and can be changed without touching the code (even while the code is running). A simple

example of ‘print.in’ may look like this:

t(F10.3)

urms(E13.4)

rhom(F10.5)

oum

which means that the output table will contain time

in the ﬁrst column formatted as

(F10.3), followed by the mean squared velocity,

urms

(i.e. hu2i1/2) in the second column

with format (E13.4), the average density

rhom

(hρi, which allows to monitor mass con-

servation) formatted (F10.5) and the kinetic helicity

oum

(that is hω·ui) in the last

column with the default format (E10.2).4The corresponding diagnostic output will look

----t---------urms--------rhom------oum----

0.000 4.9643E-03 14.42457 -8.62E-06

0.032 3.9423E-03 14.42446 -5.25E-06

0.063 6.8399E-03 14.42449 -3.50E-06

0.095 1.1437E-02 14.42455 -2.58E-06

0.126 1.6980E-02 14.42457 -1.93E-06

5.6 Data ﬁles

5.6.1 Snapshot ﬁles

Snapshot ﬁles contain the values of all evolving variables and are sufﬁcient to restart a

run. In the case of an MHD simulation with entropy equation, for example, the snapshot

ﬁles will contain the values of velocity, logarithmic density, entropy and the magnetic

vector potential.

There are two kinds of snapshot ﬁles: the current snapshot and permanent snapshots,

both of which reside in the directory ‘data/procN/’. The parameter

isav

determines the

frequency at which the current snapshot ‘data/procN/var.dat’ is written. If you keep

this frequency too high, the code will spend a lot of time on I/O, in particular for large

jobs; too low a frequency makes it difﬁcult to follow the evolution interactively during

test runs. There is also the

ialive

parameter. Setting this to 1 or 10 gives an updated

4The format speciﬁers are like in Fortran, apart from the fact that the Eformat will use standard

scientiﬁc format, corresponding to the Fortran 1pE syntax. Seasoned Fortran IV programmers may use

formats like (0pE13.4) to enjoy nostalgic feelings, or (1pF10.5) if they depend on getting wrong numbers.

26 THE PENCIL CODE

timestep in the ﬁles ‘data/proc*/alive.info’. You can put

ialive=0

to turn this off to

limit the I/O on your machine.

The permanent snapshots ‘data/proc*/VARN’ are written every

dsnap

time units. These

ﬁles are numbered consecutively from N= 1 upward and for long runs they can occupy

quite some disk space. On the other hand, if after a run you realize that some addi-

tional quantity qwould have been important to print out, these ﬁles are the only way to

reconstruct the time evolution of qwithout re-running the code.

File structure Snapshot ﬁles consist of the following

Fortran records

1. variable vector f[

nvar

]

2. time t[1], coordinate vectors x[

], y[

], z[

], grid spacings δx [1], δy [1], δz

[1], shearing-box shift ∆y[1]

All numbers (apart from the record markers) are single precision (4-byte) ﬂoating point

numbers, unless you use double precision (see §5.21, in which case all numbers are 8-

byte ﬂoating point numbers, while the record markers remain 4-byte integers.

The script pc_tsnap allows you to determine the time tof a snapshot ﬁle:

unix> pc_tsnap data/proc0/var.dat

data/proc0/var.dat: t = 8.32456

unix> pc_tsnap data/proc0/VAR2

data/proc0/VAR2: t = 2.00603

5.7 Video ﬁles and slices

We use the terms

video ﬁles

and

slice ﬁles

interchangeably. These ﬁles contain a time

series of values of one variable in a given plane. The output frequency of these video

snapshots is set by the parameter

dvid

(in code time units).

When output to video ﬁles is activated by some settings in ‘run.in’ (see example below)

and the existence of ‘video.in’, slices are written for four planes:

1. x-zplane (yindex

; ﬁle sufﬁx .xz)

2. y-zplane (yindex

; sufﬁx .yz)

3. x-yplane (yindex

; sufﬁx .xy)

4. another slice parallel to the x-yplane (yindex

iz2

; sufﬁx .xy2)

You can specify the position of the slice planes by setting the parameters

and

iz2

in the namelist

run pars

in ‘run.in’. Alternatively, you can set the input parameter

slice position

to one of ’p’ (periphery of box) or ’m’ (middle of box). Or you can also

specify the z−position in terms of z using the tags

zbot slice

and

ztop slice

. In this case,

the

zbot slice

slice will have the sufﬁx .xy and the

ztop slice

the sufﬁx .xy2

In the ﬁle ‘video.in’ of your run directory, you can choose for which variables you want

to get video ﬁles; valid choices are listed in §K.4.

Fortran record

is marked by the 4-byte integer byte count of the data in the record at the beginning

and the end, i.e. has the form hNbytes,raw data, Nbytesi

5.7 Video ﬁles and slices 27

The

slice ﬁles

are written in each processor directory ‘data/proc*/’ and have a ﬁle name

indicating the individual variable (e. g. ‘slice_uu1.yz’ for a slice of uxin the y-zplane).

Before visualizing slices one normally wants to combine the sub-slices written by each

processor into one global slice (for each plane and variable). This is done by running

‘src/read_videofiles.x’, which will prompt for the variable name, read the individual

sub-slices and write global slices to ‘data/’ Once all global slices have been assembled

you may want to remove the local slices ‘data/proc*/slice*’.

To read all sub-slices demanded in ‘video.in’ at once use ‘src/read_all_videofiles.x’.

This program doesn’t expect any user input and can thus be submitted in computing

queues.

For visualization of slices, you can use the

IDL

routines ‘rvid_box.pro’, ‘rvid_-

plane.pro’, or ‘rvid_line.pro’ which allows the ﬂag ‘/png’ for writing

PNG

images that

can then be combined into an

MPEG

movie using

mpeg encode

. Based on ‘rvid_box’,

you can write your own video routines in

IDL

An example Suppose you have set up a run using

entropy.f90

and

magnetic.f90

(most

probably together with

hydro.f90

and other modules). In order to animate slices of en-

tropy sand the z-component Bzof the magnetic ﬁeld, in planes passing through the

center of the box, do the following:

1. Write the following lines to ‘video.in’ in your run directory:

divu

2. Edit the namelist

run pars

in the ﬁle ‘run.in’. Request slices by setting

write slices

and set

dvid

and

slice position

to reasonable values, say

!lwrite_slices=T !(no longer works; write requested slices into video.in)

dvid=0.05

slice_position=’m’

3. Run the PENCIL CODE:

unix> start.csh

unix> run.csh

4. Run ‘src/read_videofiles.x’ to assemble global slice ﬁles from those scattered

across ‘data/proc*/’:

unix> src/read_videofiles.x

enter name of variable (lnrho, uu1, ..., bb3): ss

unix> src/read_videofiles.x

enter name of variable (lnrho, uu1, ..., bb3): bb3

5. Start

IDL

and run ‘rvid_box’:

unix> idl

IDL> rvid_box,’bb3’

IDL> rvid_box,’ss’,min=-0.3,max=2.

etc.

28 THE PENCIL CODE

Another example Suppose you have set up a run using

magnetic.f90

and some other

modules. This run studies some process in a “surface” layer inside the box. This “surface”

can represent a sharp change in density or turbulence. So you deﬁned your box setting

the z= 0 point at the surface. Therefore, your ‘start.in’ ﬁle will look something similar

to:

&init_pars

lperi=T,T,F

bcz = ’s’,’s’,’a’,’hs’,’s’,’s’,’a’

xyz0 = -3.14159, -3.14159, -3.14159

Lxyz = 6.28319, 6.28319, 9.42478

Now you can analyze quickly the surface of interest and some other xy−slice setting

zbot slice

and

ztop slice

in the ‘run.in’ ﬁle:

&run_pars

slice_position=’c’

zbot_slice=0.

ztop_slice=0.2

In this case, the slices with the sufﬁx .xy will be at the “surface” and the ones with the

sufﬁx .xy2 will be at the position z= 0.2above the surface. And you can visualize this

slices by:

1. Write the following lines to ‘video.in’ in your run directory:

2. Edit the namelist

run pars

in the ﬁle ‘run.in’ to include

zbot slice

and

ztop slice

3. Run the PENCIL CODE:

unix> start.csh

unix> run.csh

4. Run ‘src/read_videofiles.x’ to assemble global slice ﬁles from those scattered

across ‘data/proc*/’:

unix> src/read_videofiles.x

enter name of variable (lnrho, uu1, ..., bb3): bb3

5. Start

IDL

, load the slices with ‘pc_read_video’ and plot them at some time:

unix> idl

IDL> pc_read_video, field=’bb3’,ob=bb3,nt=ntv

IDL> tvscl,bb3.xy(*,*,100)

IDL> tvscl,bb3.xy2(*,*,100)

etc.

File structure

Slice ﬁles

consist of one Fortran record (see footnote on page 26) for

each slice, which contains the data of the variable (without ghost zones), the time tof

the snapshot and the position of the sliced variable (e. g. the xposition for a y-zslice):

1. data1[

], time t1[1], position1[1]

5.8 Averages 29

2. data2[

], time t2[1], position2[1]

3. data3[

], time t3[1], position3[1]

etc.

5.8 Averages

5.8.1 One-dimensional output averaged in two dimensions

In the ﬁle ‘xyaver.in’, z-dependent (horizontal) averages are listed. They are written to

the ﬁle ‘data/xyaverages.dat’. A new line of averages is written every

it1

th time steps.

There is the possibility to output two-dimensional averages. The result then de-

pends on the remaining dimension. The averages are listed in the ﬁles ‘xyaver.in’,

‘xzaver.in’, and ‘yzaver.in’ where the ﬁrst letters indicate the averaging directions.

The output is then stored to the ﬁles ‘data/xyaverages.dat’, ‘data/xzaverages.dat’, and

‘data/yzaverages.dat’. The output is written every

it1d

th time steps.

The rms values of the so deﬁned mean magnetic ﬁelds are referred to as

bmz

bmy

and

bmx

, respectively, and the rms values of the so deﬁned mean velocity ﬁelds are referred

to as

umz

umy

, and

umx

. (The last letter indicates the direction on which the averaged

quantity still depends.)

See Sect. 9.2 on how to add new averages.

In idl such xy-averages can be read using the procedure ‘pc_read_xyaver’.

5.8.2 Two-dimensional output averaged in one dimension

There is the possibility to output one-dimensional averages. The result then depends

on the remaining two dimensions. The averages are listed in the ﬁles ‘yaver.in’,

‘zaver.in’, and ‘phiaver.in’ where the ﬁrst letter indicates the averaging direction.

The output is then stored to the ﬁles ‘data/yaverages.dat’, ‘data/zaverages.dat’, and

‘data/phiaverages.dat’.

See Sect. 9.2 on how to add new averages.

Disadvantage: The output ﬁles, e.g. ‘data/zaverages.dat’, can be rather big because each

average is just appended to the ﬁle.

5.8.3 Azimuthal averages

Azimuthal averages are controlled by the ﬁle ‘phiaver.in’, which currently supports the

quantities listed in Sect. K.5. In addition, one needs to set

lwrite phiaverages

lwrite -

yaverages

, or

lwrite zaverages

.true.

. For example, if ‘phiaver.in’ contains the single

line

b2mphi

then you will get azimuthal averages of the squared magnetic ﬁeld B2.

30 THE PENCIL CODE

Azimuthal averages are written every

d2davg

time units to the ﬁles

‘data/averages/PHIAVGN’. The ﬁle format of azimuthal-average ﬁles consists of the

following

Fortran records

1. number of radial points Nr,φ−avg [1], number of vertical points Nz,φ−avg [1], number

of variables Nvar,φ−avg[1], number of processors in zdirection [1]

2. time t[1], positions of cylindrical radius rcyl [Nr,φ−avg] and z[Nz,φ−avg] for the grid,

radial spacing δrcyl [1], vertical spacing δz [1]

3. averaged data [Nr,φ−avg×Nz,φ−avg]

4. label length [1], labels of averaged variables [Nvar,φ−avg]

All numbers are 4-byte numbers (ﬂoating-point numbers or integers), unless you use

double precision (see §5.21).

To read and visualize azimuthal averages in

IDL

, use ‘$PENCIL_HOME/idl/files/pc_-

read_phiavg.pro’

IDL> avg = pc_read_phiavg(’data/averages/PHIAVG1’)

IDL> contour, avg.b2mphi, avg.rcyl, avg.z, TITLE=’!17B!U2!N!X’

or have a look at ‘$PENCIL_HOME/idl/phiavg.pro’ for a more sophisticated example.

5.8.4 Time averages

Time averages need to be prepared in the ﬁle ‘src/ctimeavg.local’, since they use extra

memory. They are controlled by the averaging time τavg (set by the parameter

tavg

‘run.in’), and by the indices

idx tavg

of variables to average.

Currently, averaging is implemented as exponential (memory-less) average,6

hfit+δt =hfit+δt

τavg

[f(t+δt)− hfit],(16)

which is equivalent to

hfit=

e−(t−t′)/τavg f(t′)dt′.(17)

Here t0is the time of the snapshot the calculation started with, i.e. the snapshot read by

the last run.x command. Note that the implementation (16) will approximate Eq. (17)

only to ﬁrst-order accuracy in δt. In practice, however, δt is small enough to make this

accuracy sufﬁce.

6At some point we may also implement the more straight-forward average

hfit+δt =hfit+δt

t−t0+δt[f(t+δt)− hfit],(14)

which is equivalent to

hfit=1

t−t0

f(t′)dt′,(15)

but we do not expect large differences.

5.9 Helper scripts 31

In ‘src/ctimeavg.local’, you need to set the number of slots used for time averages.

Each of these slots uses mx ×my ×mz ﬂoating-point numbers, i.e. half as much memory

as each fundamental variable.

For example, if you want to get time averages of all variables, set

integer, parameter :: mtavg=mvar

in ‘src/ctimeavg.local’, and don’t set

idx tavg

in ‘run.in’.

If you are only interested in averages of variables 1–3and 6–8(say, the velocity vector

and the magnetic vector potential in a run with ‘hydro.f90’, ‘density.f90’, ‘entropy.f90’

and ‘magnetic.f90’), then set

integer, parameter :: mtavg=6

in ‘src/ctimeavg.local’, and set

idx_tavg = 1,2,3,6,7,8 ! time-average velocity and vector potential

in ‘run.in’.

Permanent snapshots of time averages are written every

tavg

time units to

the ﬁles ‘data/proc*/TAVN’. The current time averages are saved periodically in

‘data/proc*/timeavg.dat’ whenever ‘data/proc*/var.dat’ is written. The ﬁle format for

time averages is equivalent to that of the snapshots; see §5.6.1 above.

5.9 Helper scripts

The ‘bin’ directory contains a collection of utility scripts, some of which are discussed

elsewhere, Here is a list of the more important ones.

adapt-mkﬁle Activate the settings in a ‘Makefile’ that apply to the given computer,

see §5.2.

auto-test Verify that the code compiles and runs in a set of run directories and compare

the results to the reference output. These tests are carried out routinely to ensure

that the

svn

version of the code is in a usable state.

cleanf95 Can be use to clean up the output from the Intel x86 Fortran 95 compiler

(ifc).

copy-proc-to-proc Used for restarting in a different directory. Example

copy-proc-to-proc seed.dat ../hydro256e.

copy-snapshots Copy snapshots from a processor-local directory to the global direc-

tory. To be started in the background before ‘run.x’ is invoked. Used by ‘start.csh’

and ‘run.csh’ on network connected processors.

pc copyvar var1 var2 source dest Copies snapshot ﬁles from one directory (source)

to another (dest). See documentation in ﬁle.

pc copyvar v v dir Copies all ‘var.dat’ ﬁles from current directory to ‘var.dat’ in ’dir’

run directory. Used for restarting in a different directory.

32 THE PENCIL CODE

pc copyvar N v Used to restart a run from a particular snapshot ‘VARN’. Copies a

speciﬁed snapshot ‘VARN’ to ‘var.dat’ where Nand (optionally) the target run di-

rectory are given on the command line.

cvs-add-rundir Add the current run directory to the

svn

repository.

cvsci run Similar to cvs-add-rundir, but it also checks in the ‘*.in’ and ‘src/*.local’

ﬁles. It also checks in the ﬁles ‘data/time_series.dat’, ‘data/dim.dat’ and

‘data/index.pro’ for subsequent processing in

IDL

on another machine. This is

particularly useful if collaborators want to check each others’ runs.

dx *These script perform several data collection or reformatting exercises required to

read particular ﬁles into

. They are called internally by some of the

macros

in the ‘dx/macros/’ directory.

getconf.csh See §4.3.4

gpgrowth Plot simple time evolution with Gnuplot’s ASCII graphics for fast orienta-

tion via a slow modem line.

local Materialize a symbolic link

mkcparam Based on ‘Makefile’ and ‘Makefile.local’, generate ‘src/cparam.inc’,

which speciﬁes the number

mvar

of fundamental variables, and

maux

of auxiliary

variables. Called by the ‘Makefile’.

pc mkdatadir Creates a link to a data directory in a suitable workspace. By default

this is on ‘/var/tmp/’, but different locations are speciﬁed for different machines.

mkdotin Generate minimal ‘start.in’, ‘run.in’ ﬁles based on ‘Makefile’ and

‘Makefile.local’.

mkinpars Wrapper around ‘mkdotin’ — needs proper documentation.

mkproc-tree Generates a multi-processor(‘procN’/), directory structure. Useful when

copying data ﬁles in a processor tree, such as slice ﬁles.

mkwww Generates a template HTML ﬁle for describing a run of the code, showing

input parameters and results.

move-slice Moves all the slice ﬁles from a processor tree structure, ‘procN/’, to a new

target tree creating directories where necessary.

nl2idl Transform a Fortran

namelist

(normally the ﬁles ‘param.nml’, ‘param2.nml’ writ-

ten by the code) into an

IDL

structure. Generates an

IDL

ﬁle that can be sourced

from ‘start.pro’ or ‘run.pro’.

pacx-adapt-makeﬁle Version of adapt-makeﬁle for highly distributed runs using

PACX MPI.

pc newrun Generates a new run directory from an old one. The new one contains a

copy of the old ‘*.local’ ﬁles, runs pc_setupsrc, and makes also a copy of the old

‘*.in’ and ‘k.dat’ ﬁles.

pc newscan Generates a new scan directory from an old one. The new one contains

a copy of the old, e.g. the one given under ‘samples/parameter_scan’. Look in the

‘README’ ﬁle for details.

5.10 RELOAD and STOP ﬁles 33

pc inspectrun Check the execution of the current run: prints legend and the last few

lines of the ‘time_series.dat’ ﬁle. It also appends this result to a ﬁle called ‘SPEED’,

which contains also the current wall clock time, so you can work out the speed of

the code (without being affected by i/o time).

read videoﬁles.csh The script for running read videoﬁles.x.

remote-top Create a ﬁle ‘top.log’ in the relevant ‘procN/’ directory containing the

output of top for the appropriate processor. Used in batch scripts for multi-

processor runs.

run.csh The script for producing restart ﬁles with the initial condition; see §4.3.4

scpdatadir Make a tarball of data directory, ‘data/’ and use scp to secure copy to copy

it to the speciﬁed destination.

pc setupsrc Link ‘start.csh’, ‘run.csh’ and ‘getconf.csh’ from ‘$PENCIL_HOME/bin’.

Generate ‘src/’ if necessary and link the source code ﬁles from ‘$PENCIL_HOME/src’

to that directory.

start.csh The script for initializing the code; see §4.3.4

summarize-history Evaluate ‘params.log’ and print a history of changes.

timestr Generate a unique time string that can be appended to ﬁle names from shell

scripts through the backtick mechanism.

pc tsnap Extract time information from a snapshot ﬁle, ‘VARN’.

There are several additional scripts on ‘pencil-code/utils’. Some are located in sepa-

rate folders according to users. There could be redundancies, but it is often just as easy

to write your own new script than ﬁguring out how something else works.

5.10 RELOAD and STOP ﬁles

The code periodically (every

time steps) checks for the existence of two ﬁles, ‘RELOAD’

and ‘STOP’, which can be used to trigger certain behavior.

Reloading run parameters In the directory where you started the code, create the ﬁle

‘RELOAD’ with

unix> touch RELOAD

34 THE PENCIL CODE

to force the code to re-read the runtime parameters from ‘run.in’. This will happen the

next time the code is writing monitoring output (the frequency of this happening is

controlled by the input parameter

, see Sect. 5.12).

Each time the parameters are reloaded, the new set of parameters is appended (in the

form of

namelists

) to the ﬁle ‘data/params.log’ together with the time t, so you have a

full record of your changes. If ‘RELOAD’ contains any text, its ﬁrst line will be written to

‘data/params.log’ as well, which allows you to annotate changes:

unix> echo "Reduced eta to get fields growing" > RELOAD

Use the command summarize-history to print a history of changes.

Stopping the code In the directory where you started the code, create the ﬁle ‘STOP’

with

unix> touch STOP

to stop the code in a controlled manner (it will write the latest snapshot). Again, the

action will happen the next time the code is writing monitoring output.

5.11 RERUN and NEWDIR ﬁles

After the code ﬁnishes (e.g., when the ﬁnal timestep number is reached or when a ‘STOP’

ﬁle is found), the ‘run.csh’ script checks whether there is a ‘RERUN’ ﬁle. If so, the code will

simply run again, perhaps even after you have recompiled the code. This is useful in the

development phase when you changed something in the code, so you don’t need to wait

for a new slot in the queue!

Even more naughty, as Tony says, is the ‘NEWDIR’ ﬁle, where you can enter a new direc-

tory path (relative path is ok, e.g. ../conv-slab). If nothing is written in this ﬁle (e.g.

via touch NEWDIR) it stays in the same directory. On distributed machines, the ‘NEWDIR’

method will copy all the ‘VAR#’ and ‘var.dat’ ﬁles back to and from the sever. This can be

useful if you want to run with new data ﬁles, but you better do it in a separate directory,

because with ‘NEWDIR’ the latest data from the code are written back to the server before

running again.

Oh, by the way, if you want to be sure that you haven’t messed up the content of the pair

of ‘NEWDIR’ ﬁles, you may want to try out the pc_jobtransfer command. It writes the

decisive ‘STOP’ ﬁle only after the script has checked that the content of the two ‘NEWDIR’

ﬁles points to existing run directory paths, so if the new run crashes, the code returns

safely to the old run directory. I’m not sure what Tony would say now, but this is now

obviously extremely naughty.

5.12 Start and run parameters

All input parameters in ‘start.in’ and ‘run.in’ are grouped in Fortran

namelists

. This

allows arbitrary order of the parameters (within the given namelist; the namelists need

no longer be in the correct order), as well as enhanced readability through inserted For-

tran comments and whitespace. One namelist (

init pars

run pars

) contains general

parameters for initialization/running and is always read in. All other namelists are spe-

ciﬁc to individual modules and will only be read if the corresponding module is used.

5.12 Start and run parameters 35

The syntax of a namelist (in an input ﬁle like ‘start.in’) is

&init_pars

ip=5, Lxyz=2,4,2

— in this example, the name of the namelist is

init pars

, and we read just two variables

(all other variables in the namelist retain their previous value):

, which is set to 5, and

Lxyz

, which is a vector of length three and is set to (2,4,2).

While all parameters from the namelists can be set, in most cases reasonable default

values are preset. Thus, the typical ﬁle ‘start.in’ will only contain a minimum set of

variables or (if you are very minimalistic) none at all. If you want to run a particular

problem, it is best to start by modifying an existing example that is close to your appli-

cation.

Before starting a simulation run, you may want to execute the command pc_configtest

in order to test the correctness of your changes to these conﬁguration ﬁles.

As an example, we give here the start parameters for ‘samples/helical-MHDturb’

&init_pars

cvsid=’$Id:$’, ! identify version of start.in

xyz0 = -3.1416, -3.1416, -3.1416, ! first corner of box

Lxyz = 6.2832, 6.2832, 6.2832, ! box size

lperi = T , T , T , ! periodic in x, y, z

random_gen=’nr_f90’

&hydro_init_pars

&density_init_pars

gamma=1.

&magnetic_init_pars

initaa=’gaussian-noise’, amplaa=1e-4

The three entries specifying the location, size and periodicity of the box are just given

for demonstration purposes here — in fact a periodic box from −πto −πin all three

directions is the default. In this run, for reproducibility, we use a random number gen-

erator from the Numerical Recipes [31], rather than the compiler’s built-in generator.

The adiabatic index γis set explicitly to 1(the default would have been 5/3) to achieve

an isothermal equation of state. The magnetic vector potential is initialized with uncor-

related, normally distributed random noise of amplitude 10−4.

The run parameters for ‘samples/helical-MHDturb’ are

&run_pars

cvsid=’$Id:$’, ! identify version of start.in

nt=10, it1=2, cdt=0.4, cdtv=0.80, isave=10, itorder=3

dsnap=50, dvid=0.5

random_gen=’nr_f90’

&hydro_run_pars

36 THE PENCIL CODE

&density_run_pars

&forcing_run_pars

iforce=’helical’, force=0.07, relhel=1.

&magnetic_run_pars

eta=5e-3

&viscosity_run_pars

nu=5e-3

Here we run for

= 10 timesteps, every second step, we write a line of diagnostic output;

we require the time step to keep the advective

Courant number

≤0.4and the diffusive

Courant number

≤0.8, save ‘var.dat’ every 20 time steps, and use the 3-step time-

stepping scheme described in Appendix H.4 (the Euler scheme

itorder

= 1 is only useful

for tests). We write permanent snapshot ﬁle ‘VARN’ every

dsnap

= 50 time units and 2d

slices for animation every

dvid

= 0.5time units. Again, we use a deterministic random

number generator. Viscosity νand magnetic diffusivity ηare set to 5×10−3(so the mesh

Reynolds number is about urmsδx/ν = 0.3×(2π/32)/5×10−3≈12, which is in fact rather a

bit to high). The parameters in

forcing run pars

specify fully helical forcing of a certain

amplitude.

A full list of input parameters is given in Appendix K.

5.13 Physical units

Many calculations are unit-agnostic, in the sense that all results remain the same in-

dependent of the unit system in which you interpret the numbers. E. g. if you simulate

a simple hydrodynamical ﬂow in a box of length L= 1.and get a maximum velocity of

umax = 0.5after t= 3 time units, then you may interpret this as L= 1 m,umax = 0.5 m/s,

t= 3 s, or as L= 1 pc,umax = 0.5 pc/Myr,t= 3 Myr, depending on the physical system you

have in mind. The units you are using must of course be consistent, thus in the second

example above, the units for diffusivities would be pc2/Myr, etc.

The units of magnetic ﬁeld and temperature are determined by the values µ0= 1 and

cp= 1 used internally by the code7. This means that if your units for density and velocity

are [ρ]and [v], then magnetic ﬁelds will be in

[B] = pµ0[ρ] [v]2,(18)

and temperatures are in

[T] = [v]2

=γ−1

[v]2

R/µ .(19)

For some choices of density and velocity units, Table 2 shows the resulting units of

magnetic ﬁeld and temperature.

7Note that cp= 1 is only assumed if you use the module

noionization.f90

. If you work with

ioniza-

tion.f90

, temperature units are speciﬁed by

unit temperature

as described below.

5.14 Minimum amount of viscosity 37

Table 2: Units of magnetic ﬁeld and temperature for some choices of [ρ]and [v]according to Eqs. (18) and

(19). Values are for a monatomic gas (γ= 5/3) of mean atomic weight ¯µg= ¯µ/1 g in grams.

[ρ] [v] [B] [T]

1 kg/m31 m/s 1.12 mT = 11.2 G ¯µg

0.6×2.89 ×10−5K

1 g/cm31 cm/s 3.54 ×10−4T = 3.54 G ¯µg

0.6×2.89 nK

1 g/cm31 km/s 35.4 T = 354 kG ¯µg

0.6×28.9 K

1 g/cm310 km/s 354 T = 3.54 MG ¯µg

0.6×2 890 K

On the other hand, as soon as material equations are used (e.g. one of the popular pa-

rameterizations for radiative losses, Kramers opacity, Spitzer conductivities or ioniza-

tion, which implies well-deﬁned ionization energies), the corresponding routines in the

code need to know the units you are using. This information is speciﬁed in ‘start.in’ or

‘run.in’ through the parameters

unit system

unit length

unit velocity

unit density

and

unit temperature

8like e. g.

unit_system=’SI’,

unit_length=3.09e16, unit_velocity=978. ! [l]=1pc, [v]=1pc/Myr

Note: The default unit system is unit_system=’cgs’ which is a synonym for unit_-

system=’Babylonian cubits’.

5.14 Minimum amount of viscosity

We emphasize that, by default, the code works with constant diffusion coefﬁcients (vis-

cosity ν, thermal diffusivity χ, magnetic diffusivity η, or passive scalar diffusivity D).

If any of these numbers is too small, you would need to have more meshpoints to get

consistent numerical solutions; otherwise the code develops wiggles (‘ringing’) and will

eventually crash. A useful criterion is given by the mesh Reynolds number based on the

maximum velocity,

Remesh = max(|u|) max(δx, δy, δz)/ν, (20)

which should not exceed a certain value which can be problem-dependent. Often the

largest possible value of Remesh is around 5. Similarly there exist mesh P´

eclet and mesh

magnetic Reynolds numbers that should not be too large.

Note that in some cases, ‘wiggles’ in ln ρwill develop despite sufﬁciently large diffusion

coefﬁcients, essentially because the continuity equation contains no dissipative term.

For convection runs (but not only for these), we have found that this can often be pre-

vented by

upwinding

, see Sect. H.2.

If the Mach number of the code approaches unity, i.e. if the rms velocity becomes com-

parable with the speed of sound, shocks may form. In such a case the mesh Reynolds

number should be smaller. In order to avoid excessive viscosity in the unshocked regions,

8Note: the parameter

unit temperature

is currently only used in connection with

ionization.f90

. If you

are working with

noionization.f90

, the temperature unit is completely determined by Eq. (19) above.

38 THE PENCIL CODE

one can use the so-called shock viscosity (Sect. 6.6.1) to concentrate the effects of a low

mesh Reynolds number to only those areas where it is necessary.

5.15 The time step

5.15.1 The usual RK-2N time step

RK-2N refers to the third order Runge-Kutta scheme by Williamson (1980) with a mem-

ory consumption of two chunks. Therefore the 2N in the name.

The time step is normally speciﬁed as Courant time step through the coefﬁcients

cdt

(cδt),

cdtv

(cδt,v) and

cdts

(cδt,s). The resulting Courant step is given by

δt = min cδt

δxmin

Umax

, cδt,v

δx2

min

Dmax

, cδt,s

Hmax ,(21)

where

δxmin ≡min(δx, δy, δz) ; (22)

Umax ≡max |u|+qc2

s+v2

A,(23)

csand vAdenoting sound speed and Alfv´

en speed, respectively;

Dmax = max(ν, γχ, η, D),(24)

where νdenotes kinematic viscosity, χ=K/(cpρ)thermal diffusivity and ηthe magnetic

diffusivity; and

Hmax = max 2νS2+ζshock(∇·u)2+...

cvT,(25)

where dots indicate the presence of other terms on the rhs of the entropy equation.

To ﬁx the time step δt to a value independent of velocities and diffusivities, explicitly set

the run parameter

, rather than

cdt

cdtv

(see p. 182).

If the time step exceeds the viscous time step the simulation may actually run ok for

quite some time. Inspection of images usually helps to recognize the problem. An exam-

ple is shown in Fig. 4.

Timestepping is accomplished using the Runge-Kutta 2N scheme. Regarding details of

this scheme see Sect. H.4.

5.15.2 The Runge-Kutta-Fehlberg time step

A ﬁfth order Runge-Kutta-Fehlberg time stepping procedure is available. It is used

mostly for chemistry application, often together with the double precision option. In

order to make this work, you need to compile with

TIMESTEP = timestep_rkf

in ‘src/Makefile.local’. In addition, you must put

itorder=5

in ‘run.in’. An example

application is ‘samples/1d-tests/H2_flamespeed’. This procedure is still experimental.

5.16 Boundary conditions 39

Figure 4: Example of a velocity slice from a run where the time step is too long. Note the spurious

checkerboard modulation in places, for example near x=−0.5and −2.5< y < −1.5. This is an example

of a hyperviscous turbulence simulations with 5123meshpoints and a third order hyperviscosity of ν3=

5×10−12. Hyperviscosity is explained in the Appendix E.

5.16 Boundary conditions

5.16.1 Where to specify boundary conditions

In most tests that come with the PENCIL CODE, boundary conditions are set in ‘run.in’,

which is a natural choice. However, this may lead to unexpected initial data written by

‘start.x’, since when you start the code (via ‘start.csh’), the boundary conditions are

unknown and ‘start.x’ will then ﬁll the ghost zones assuming periodicity (the default

boundary condition) in all three directions. These ghost data will never be used in a

calculation, as ‘run.x’ will apply the boundary conditions before using any ghost-zone

values.

To avoid these periodic conditions in the initial snapshot, you can set the boundary

conditions in ‘start.in’ already. In this case, they will be inherited by ‘run.x’, unless you

also explicitly set boundary conditions in ‘run.in’.

5.16.2 How to specify boundary conditions

Boundary conditions are implemented through three layers of

ghost points

on either

boundary, which is quite a natural choice for an MPI code that uses ghost zones for

representing values located on the neighboring processors anyway. The desired type of

boundary condition is set through the parameters

{

x,y,z

}in ‘run.in’; the nomenclature

used is as follows. Set

{

x,y,z

}to a sequence of letters like

bcx = ’p’,’p’,’p’, ’p’, ’p’

for periodic boundaries, or

bcz = ’s’,’s’,’a’,’a2’,’c1:c2’

for non-periodic ones. Each element corresponds to one of the variables, which are those

of the variables ux,uy,uz,ln ρ,s/cp,Ax,Ay,Az,ln cthat are actually used in this order.

The following conditions are available:

‘p’periodic boundary condition

‘a’antisymmetric condition w. r. t. the boundary, i. e. vanishing value

40 THE PENCIL CODE

‘s’symmetric condition w. r. t. the boundary, i. e. vanishing ﬁrst derivative

‘a2’antisymmetry w. r. t. the arbitrary value on the boundary, i. e. vanishing second

derivative

‘c1’special boundary condition for ln ρand s: constant heat ﬂux through the boundary

‘c2’special boundary condition for s: constant temperature at the boundary — requires

boundary condition a2 for ln ρ

‘cT’special boundary condition for sor ln T: constant temperature at the boundary (for

arbitrarily set ln ρ)

‘ce’special boundary condition for s: set temperature in ghost points to value on bound-

ary (for arbitrarily set ln ρ)

‘db’low-order one-sided derivatives (“no boundary condition”) for density

‘she’shearing-sheet boundary condition (default when the module

Shear

is used)

‘g’force the value of the corresponding ﬁeld on vertical boundaries (should be used

in combination with the force lower bound and force upper bound ﬂags set in the

namelist init pars)

‘hs’special boundary condition for ln ρand swhich enforces hydrostatic equilibrium on

vertical boundaries

The extended syntax a:b(e. g. ‘c1:c2’) means: use boundary condition aat the left/lower

boundary, but bat the right/upper one.

If you build a new ‘run.in’ ﬁle from another one with a different number of variables

(

noentropy

vs.

entropy

, for example), you need to remember to adjust the length of the

arrays

bcx

bcz

. The advantage of the present approach is that it is very easy to ex-

change all boundary conditions by a new set of conditions in a particular direction (for

example, make everything periodic, or switch off shearing sheet boundary conditions

and have stress-free instead).

5.17 Restarting a simulation

When a run stops at the end of a simulation, you can just resubmit the job again, and

it will start from the latest snapshot saved in ‘data/proc*/var.dat’. The value of the

latest time is saved in a separate ﬁle, ‘data/proc*/time.dat’. On parallel machines it is

possible that some (or just one) of the ‘var.dat’ are corrupt; for example after a system

crash. Check for ﬁle size and date, and restart from a good ‘VAR’Nﬁle instead.

If you want to run on a different machine, you just need to copy the ‘data/proc*/var.dat’

(and, just to be sure) ‘data/proc*/time.dat’) ﬁles into a new directory tree. You may also

need the ‘data/proc*/seed.dat’ ﬁles for the random number generator. The easiest way

to get all these other ﬁles is to run start.csh again on the new machine (or in a new

directory) and then to overwrite the ‘data/proc*/var.dat’ ﬁles with the correct ones.

For restarting from runs that didn’t have magnetic ﬁelds, passive scalar ﬁelds, or test

ﬁelds, see Sect. F.3.

5.18 One- and two-dimensional runs 41

5.18 One- and two-dimensional runs

If you want to run two-dimensional problems, set the number of mesh points in one

direction to unity, e.g.

nygrid

=1 or

nzgrid

=1 in ‘cparam.local’. Remember that the num-

ber of mesh points is still divisible by the number of processors. For 2D-runs, it is also

possible to write only 2D-snapshots (i.e. VAR ﬁles written only in the considered (x, y)

or (x, z)plane, with a size seven times smaller as we do not write the third unused di-

rection). To do that, please add the logical ﬂag ‘lwrite 2d=T’ in the namelist init pars in

‘start.in’.

Similarly, for one-dimensional problems, set, for example,

nygrid

=1 and

nzgrid

=1 in

‘cparam.local’. You can even do a zero-dimensional run, but then you better set

(rather than

cdt

), because there is no Courant condition for the time step.

See 0d, 1d, 2d, and 3d tests with examples.

5.19 Visualization

5.19.1 Gnuplot

Simple visualization can easily be done using

Gnuplot

(http://www.gnuplot.info), an

open-source plotting program suitable for two-dimensional plots.

For example, suppose you have the variables

---it-----t-------dt-------urms-----umax-----rhom-----ssm------dtc---

in ‘time_series.dat’ and want to plot urms(t). Just start gnuplot and type

gnuplot> plot "data/time_series.dat" using 2:4 with lines

If you work over a slow line and want to see both urms(t)and umax(t), use ASCII graphics:

gnuplot> set term dump

gnuplot> set logscale y

gnuplot> plot "data/time_series.dat" using 2:4 title "urms", \

gnuplot> "data/time_series.dat" using 2:5 title "umax"

5.19.2 Data explorer

(

data explorer

;http://www.opendx.org) is an open-source tool for visualization of

three-dimensional data.

The PENCIL CODE provides a few networks for

. It is quite easy to read in a snapshot

ﬁle from

(the only tricky thing is the four extra bytes at the beginning of the ﬁle,

representing a Fortran record marker), and whenever you run ‘start.x’, the code writes

a ﬁle ‘var.general’ that tells

all it needs to know about the data structure.

As a starting point for developing your own

programs or

networks

, you can use a

few generic

scripts provided in the directory ‘dx/basic/’. From the run directory,

start

with

unix> dx -edit $PENCIL_HOME/dx/basic/lnrho

42 THE PENCIL CODE

to load the ﬁle ‘dx/basic/lnrho.net’, and execute it with ✄

✂



✁

Ctl-o or Execute →Execute

Once. You will see a set of iso-surfaces of logarithmic density. If the viewport does not

ﬁt to your data, you can reset it with ✄

✂



✁

Ctl-f. To rotate the object, drag the mouse over

the Image window with the left or right mouse button pressed. Similar networks are

provided for entropy (‘ss.net’), velocity (‘uu.net’) and magnetic ﬁeld (‘bb.net’).

When you expand these simple networks to much more elaborate ones, it is probably

a good idea to separate the different tasks (like Importing and Selecting, visualizing

velocity, visualizing entropy, and Rendering) onto separate pages through Edit →Page.

Note Currently,

can only read in data ﬁles written by one single processor, so from

a multi-processor run, you can only visualize one subregion at a time.

5.19.3 GDL

GDL

, also known as

Gnu Data Language

is a free visualization package that can be

found at http://gnudatalanguage.sourceforge.net/. It aims at replacing the very ex-

pensive

IDL

package (see S. 5.19.4). For the way we use IDL for the Pencil Code, com-

patibility is currently not completely sufﬁcient, but you can use GDL for many of the

visualization tasks. If you get spurious “Error opening ﬁle” messages, you can normally

simply ignore them.

This section tells you how to get started with using GDL for visualization.

Setup As of GDL 0.9 – at least the version packed with Ubuntu Jaunty (9.10) – you

will need to add GDL’s ‘examples/pro/’ directory to your

!PATH

variable. So the ﬁrst call

after starting

GDL

should be

GDL> .run setup_gdl

Starting visualization There are mainly two possibilities for visualization: using a sim-

ple GUI or loading the data with pc_read and work with it interactively. Please note that

the GUI was written and tested only with IDL, see §5.19.4.

Here, the pc_read family of IDL routines to read the data is described. Try

GDL> pc_read

to get an overview.

To plot a time series, use

GDL> pc_read_ts, OBJECT=ts

GDL> help, ts, /STRUCT ;; (to see which slots are available)

GDL> plot, ts.t, ts.umax

GDL> oplot, ts.t, ts.urms

Alternatively, you could simply use the ‘ts.pro’ script:

GDL> .run ts

To work with data from ‘var.dat’ and similar snapshot ﬁles, you can e.g. use the follow-

ing routines:

5.19 Visualization 43

GDL> pc_read_dim, OBJECT=dim

GDL> $$PENCIL_HOME/bin/nl2idl -d ./data/param.nml> ./param.pro

GDL> pc_read_param, OBJECT=par

GDL> pc_read_grid, OBJECT=grid

GDL> pc_read_var, OBJECT=var

Having thus read the data structures, we can have a look at them to see what informa-

tion is available:

GDL> help, dim, /STRUCT

GDL> help, par, /STRUCT

GDL> help, grid, /STRUCT

GDL> help, var, /STRUCT

To visualize data, we can e.g. do9

GDL> plot, grid.x, var.ss[*, dim.ny/2, dim.nz/2]

GDL> contourfill, var.ss[*, *, dim.nz/2], grid.x, grid.y

GDL> ux_slice = var.uu[*, *, dim.nz/2, 0]

GDL> uy_slice = var.uu[*, *, dim.nz/2, 1]

GDL> wdvelovect, ux_slice, uy_slice, grid.x, grid.y

GDL> surface, var.lnrho[*, *, dim.nz/2, 0]

See also Sect. 5.19.4.

5.19.4 IDL

IDL

is a commercial visualization program for two-dimensional and simple three-

dimensional graphics. It allows to access and manipulate numerical data in a fashion

quite similar to how Fortran handles them.

In ‘$PENCIL_HOME/idl’, we provide a number of general-purpose

IDL

scripts that we are

using all the time in connection with the PENCIL CODE. While

IDL

is quite an expensive

software package, it is quite useful for visualizing results from numerical simulations.

In fact, for many applications, the 7-minute demo version of

IDL

is sufﬁcient.

Visualization in IDL The Pencil Code GUI is a data post-processing tool for the usage

on a day-to-day basis. It allows fast inspection of many physical quantities, as well as ad-

vanced features like horizontal averages, streamline tracing, freely orientable 2D-slices,

and extraction of cut images and movies. To use the Pencil Code GUI, it is sufﬁcient to

run:

unix> idl

IDL> .r pc_gui

If you like to load only some subvolume of the data, like any 2D-slices from the given

data snapshots, or 3D-subvolumes, it is possible to choose the corresponding options in

the ﬁle selector dialog. The Pencil Code GUI offers also some options to be set on the

command-line, please refer to their description in the source code.

9If contourfill produces just contour lines instead of a color-coded plot, your version of GDL is too

old. E.g. the version shipped with Ubuntu 9.10 is based on GDL 0.9rc1 and has this problem.

44 THE PENCIL CODE

There are also other small GUIs available, e.g. the ﬁle ‘time-series.dat’ can easily be

analyzed with the command:

unix> idl

IDL> pc_show_ts

The easiest way to derive physical quantities at the command-line is to use one of the

many pc_read_var-variants (pc_read_var_raw is recommended for large datasets be-

cause of its high efﬁciency regarding computation and memory usage) for reading the

data. With that, one can make use of pc_get_quantity to derive any implemented physi-

cal quantity. Packed in a script, this is the recommended way to get reproducible results,

without any chance for accidental errors on the interactive IDL command-line.

Alternatively, by using the command-line to see the time evolution of e.g. velocity and

magnetic ﬁeld (if they are present in you run), start

IDL

10 and run ‘ts.pro’:

unix> idl

IDL> .run ts

The

IDL

script ‘ts.pro’ reads the time series data from ‘data/time_series.dat’ and sorts

the column into the structure

, with the slot names corresponding to the name of the

variables (taken from the header line of ‘data/time_series.dat’). Thus, you can refer to

time as ts.t, to the rms velocity as ts.urms, and in order to plot the mean density as a

function of time, you would simply type

IDL> plot, ts.t, ts.rhom

The basic command sequence for working with a snapshot is:

unix> idl

IDL> .run start

IDL> .run r

IDL>

[speciﬁc commands]

You run ‘start.pro’ once to initialize (or reinitialize, if the mesh size has changed, for

example) the ﬁelds and read in the startup parameters from the code. To read in a new

snapshot, run ‘r.pro’ (or ‘rall.pro’, see below).

If you are running in parallel on several processors, the data are scattered over different

directories. To reassemble everything in

IDL

, use

10 If you run IDL from the command line, you will highly appreciate the following tip: IDL’s command

line editing is broken beyond hope. But you can ﬁx it, by running IDL under rlwrap, a wrapper for the

excellent GNU

readline

library.

Download and install rlwrap from http://utopia.knoware.nl/~hlub/uck/rlwrap/ (on some systems

you just need to run ‘emerge rlwrap’, or ‘apt-get install rlwrap’), and alias your idl command:

csh> alias idl ’rlwrap -a -c idl’

bash> alias idl=’rlwrap -a -c idl’

From now on, you can

•use long command lines that correctly wrap around;

•type the ﬁrst letters of a command and then ✄

✂



✁

PageUp to recall commands starting with these letters;

•capitalize, uppercase or lowercase a word with ✄

✂



✁

Esc-C, ✄

✂



✁

Esc-U, ✄

✂



✁

Esc-L;

•use command line history across IDL sessions (you might need to create ‘~/.idl_history’ for this);

•complete ﬁle names with ✄

✂



✁

Tab (works to some extent);

•. . . use all the other

readline

features that you are using in bash,octave,bc,gnuplot,ftp, etc.

5.19 Visualization 45

IDL> .r rall

instead of .r r (here, .r is a shorthand for .run). The procedure ‘rall.pro’ reads (and

assembles) the data from all processors and correspondingly requires large amounts of

memory for very large runs. If you want to look at just the data from one processor, use

‘r.pro’ instead.

If you need the magnetic ﬁeld or the current density, you can calculate them in IDL by

IDL> bb=curl(aa)

IDL> jj=curl2(aa)

By default one is reading always the current snapshot ‘data/procN/var.dat’; if you want

to read one of the permanent snapshots, use (for example)

IDL> varfile=’VAR2’

IDL> .r r

(or

.r rall

)

See Sect. 5.6.1 for details on permanent snapshots.

With ‘r.pro’, you can switch the part of the domain by changing the variable

datadir

IDL> datadir=’data/proc3’

IDL> .r r

will read the data written by processor 3.

Reading data into IDL arrays or structures As an alternative to the method described

above, there is also the possibility to read the data into structures. This makes some

more operations possible, e.g. reading data from an IDL program where the command

.r is not allowed.

An efﬁcient and still scriptable way would look like the following:

IDL> pc_read_var_raw, obj=var, tags=tags

IDL> bb = pc_get_quantity (’B’, var, tags)

IDL> jj = pc_get_quantity (’j’, var, tags)

This reads the data into an array ‘var’, as well as the array indices of the contained phys-

ical variables into a separate structure ‘tags’. To use a caching mechanism within pc_-

get_quantity, please refer to the documentation and the examples contained in ‘pencil-

code/idl/pc get quantity.pro’, where you can also start adding not yet implemented phys-

ical quantities.

To read a snapshot ’VAR10’ into the IDL structure ff, type the following command

IDL> pc_read_var, obj=ff, varfile=’VAR10’, /trimall

The option /trimall removes ghost zones from the data. A number of other options are

documented in the source code of pc_read_var. You can see what data the structure

contains by using the command tag_names

IDL> print, tag_names(ff)

T X Y Z DX DY DZ UU LNRHO AA

11 Keep in mind that jj=curl(bb) would use iterated ﬁrst derivatives instead of the second derivatives

and thus be numerically less accurate than jj=curl2(aa), particularly at small scales.

46 THE PENCIL CODE

One can access the individual variables by typing ff.varname, e.g.

IDL> help, ff.aa

<Expression> FLOAT = Array[32, 32, 32, 3]

There are a number of ﬁles that read different data into structures. They are placed

in the directory \$PENCIL_HOME/idl/files. Here is a list of ﬁles (including suggested

options to call them with)

•pc_read_var_raw, obj=var, tags=tags

Efﬁciently read a snapshot into an array.

•pc_read_var, obj=ff, /trimall

Read a snapshot into a structure.

•pc_read_ts, obj=ts

Read the time series into a structure.

•pc_read_xyaver, obj=xya

pc_read_xzaver, obj=xza

pc_read_yzaver, obj=yza

Read 1-D time series into a structure.

•pc_read_const, obj=cst

Read code constants into a structure.

•pc_read_pvar, obj=fp

Read particle data into a structure.

•pc_read_param, obj=par

Read startup parameters into a structure.

•pc_read_param, obj=par2, /param2

Read runtime parameters into a structure.

Other options are documented in the source code of the ﬁles.

For some examples on how to use these routines, see Sect. 5.19.3.

5.19.5 Python

Pencil supports reading, processing and the visualization of data using

python

. A num-

ber of scripts are placed in the subfolder ‘$PENCIL_HOME/python’. A README ﬁle placed

under that subfolder contains the information needed to read Pencil output data into

python.

Installation For modern operating systems, Python is generally installed together with

the system. If not, it can be installed via your preferred package manager or downloaded

from the website https://www.python.org/. For convenience, it is strongly recommend

to also install IPython, which is a more convenient console for Python. You will also need

the NumPy, matplotlib and Tk library.

Perhaps the easiest way to obtain all the required software mentioned above is to install

either Continuum’s Anaconda or Enthought’s Canopy. These Python distributions also

provide (or indeed are) integrated graphical development environments.

5.19 Visualization 47

In order for Python to ﬁnd the Pencil Code commands you will have to add to your

.bashrc:

export PYTHONPATH=$PENCIL_HOME/python

ipythonrc If you use IPython, for convenience, you should modify your

.ipython/ipythonrc (create it if it doesn’t exist) and add:

import_all pencil

Additional, add to your .ipython/profile_default/startup/init.py the following lines:

import numpy as np

import pylab as plt

import pencil as pc

import matplotlib

from matplotlib import rc

plt.ion()

matplotlib.rcParams[’savefig.directory’] = ’’

.pythonrc In case you are on a cluster and don’t have access to IPython you can edit

your .pythonrc:

#!/usr/bin/python

import numpy as np

import pylab as plt

import pencil as pc

import atexit

#import readline

import rlcompleter

# enables search with CTR+r in the history

try:

import readline

except ImportError:

print "Module readline not available."

else:

import rlcompleter

readline.parse_and_bind("tab: complete")

# enables command history

historyPath = os.path.expanduser("~/.pyhistory")

def save_history(historyPath=historyPath):

import readline

readline.write_history_file(historyPath)

if os.path.exists(historyPath):

readline.read_history_file(historyPath)

atexit.register(save_history)

del os, atexit, readline, rlcompleter, save_history, historyPath

plt.ion()

48 THE PENCIL CODE

create the ﬁle .pythonhistory and add to your .bashrc:

export PYTHONSTARTUP=~/.pythonrc

Pencil Code Commands in General For a list of all Pencil Code commands start

IPython and type pc. <TAB> (as with auto completion). To access the help of any com-

mand just type the command followed by a ’?’ (no spaces), e.g.:

In [1]: pc.dot?

Type: function

String Form:<function dot at 0x7f9d96cb0cf8>

File: ~/pencil-code/python/pencil/math/vector_multiplication.py

Definition: pc.dot(a, b)

Docstring:

take dot product of two pencil-code vectors a & b with shape

a.shape = (3,mz,my,mx)

You can also use help(pc.dot) for a more complete documentation of the command.

There are various reading routines for the Pencil Code data. All of them return an object

with the data. To store the data into a user deﬁned variable type e.g.

In [1]: ts = pc.read_ts()

Most commands take some arguments. For most of them there is a default value, e.g.

In [1]: pc.read_ts(filename=’time_series.dat’, datadir=’data’, plot_data=True)

You can change the values by simply typing e.g.

In [1]: pc.read_ts(plot_data = False)

Reading and Plotting Time Series Reading the time series ﬁle is very easy. Simply

type

In [1]: ts = pc.read_ts()

and Python stores the data in the variable ts. The physical quantities are members of

the object ts and can be accessed accordingly, e.g. ts.t,ts.emag. To check which other

variables are stored simply do the tab auto completion ts. <TAB>.

Plot the data with the matplotlib commands:

In [1]: plt.plot(ts.t, ts.emag)

The standard plots are not perfect and need a little polishing. See

the online wiki for a few examples on how to make pretty plots

(https://github.com/pencil-code/pencil-code/wiki/PythonForPencil). You can

save the plot into a ﬁle using the GUI or with

In [1]: plt.savefig(’plot.eps’)

Reading and Plotting VAR ﬁles and slice ﬁles Read var ﬁles:

In [1]: var = pc.read_var()

5.20 Running on multi-processor computers 49

Read slice ﬁles:

In [1]: slices, t = pc.read_slices(field=’bb1’, extension=’xy’)

This returns the array slices with indices slices[nTimes, my, mx] and the time array

If you want to plot e.g. the x-component of the magnetic ﬁeld at the central plane simply

type:

In [1]: plt.imshow(zip(*var.bb[0, 128, :, :]), origin=’lower’, extent=[-4, 4, -4, 4])

For a complete list of arguments of plt.imshow refer to its documentation.

For a more interactive plot use:

In [1]: pc.animate_interactive(slices, t)

Be aware: arrays from the reading routines are ordered f[nvar, mz, my, mx], i.e. re-

versed to IDL. This affects reading var ﬁles and slice ﬁles.

5.20 Running on multi-processor computers

The code is parallelized using

MPI

(

message passing interface

) for a simple domain

decomposition (data-parallelism), which is a straight-forward and very efﬁcient way of

parallelizing ﬁnite-difference codes. The current version has a few restrictions, which

need to be kept in mind when using the MPI features.

The global number of grid points (but excluding the ghost zones) in a given direction

must be an exact multiple of the number of processors you use in that direction. For

example if you have nprocy=8 processors for the ydirection, you can run a job with

nygrid=64 points in that direction, but if you try to run a problem with nygrid=65 or

nygrid=94, the code will complain about an inconsistency and stop. (So far, this has not

been a serious restriction for us.)

5.20.1 How to run a sample problem in parallel

To run the sample problem in the directory ‘samples/conv-slab’ on 16 CPUs, you need

to do the following (in that directory):

1. Edit ‘src/Makefile.local’ and replace

MPICOMM = nompicomm

MPICOMM = mpicomm

2. Edit ‘src/cparam.local’ and replace

integer, parameter :: ncpus=1, nprocy=1, nprocz=ncpus/nprocy, nprocx=1

integer, parameter :: nxgrid=32, nygrid=nxgrid, nzgrid=nxgrid

integer, parameter :: ncpus=16, nprocy=4, nprocz=ncpus/nprocy, nprocx=1

integer, parameter :: nxgrid=128, nygrid=nxgrid, nzgrid=nxgrid

50 THE PENCIL CODE

The ﬁrst line speciﬁes a 4×4layout of the data in the yand zdirection. The second

line increases the resolution of the run because running a problem as small as 323

on 16 CPUs would be wasteful. Even 1283may still be quite small in that respect.

For performance timings, one should try and keep the size of the problem per CPU

the same, so for example 2563on 16 CPUs should be compared with 1283on 2 CPUs.

3. Recompile the code

unix> (cd src; make)

4. Run it

unix> start.csh

unix> run.csh

Make sure that all CPUs see the same ‘data/’ directory; otherwise things will go wrong.

Remember that in order to visualize the full domain with IDL (rather than just the

domain processed and written by one processor), you need to use ‘rall.pro’ instead of

‘r.pro’.

5.20.2 Hierarchical networks (e.g. on Beowulf clusters)

On big Beowulf clusters, a group of nodes is often connected with a switch of modest

speed, and all these groups are connected via a ntimes faster uplink switch. When

bandwidth-limited, it is important to make sure that consecutive processors are mapped

onto the mesh such that the load on the uplink is .ntimes larger than the load on the

slower switch within each group. On a 512 node cluster, where groups of 24 processors

are linked via fast ethernet switches, which in turn are connected via a Gigabit uplink

(∼10 times faster), we found that

nprocy

=4 is optimal. For 128 processors, for example

we ﬁnd that

nprocy

nprocz

= 4×32 is the optimal layout, while. For comparison, 8×16

is 3 times slower, and 16 ×8is 17 (!) times slower. These results can be understood from

the structure of the network, but the basic message is to watch out for such effects and

to try varying

nprocy

and

nprocz

In cases where nygrid>nzgrid it may be advantageous to swap the ordering of processor

numbers. This can be done by setting

lprocz slowest

=F.

5.20.3 Extra workload caused by the ghost zones

Normally, the workload caused by the ghost zones is negligible. However, if one increases

the number of processors, a signiﬁcant fraction of work is done in the ghost zones. In

other words, the effective mesh size becomes much larger than the actual mesh size.

Consider a mesh of size Nw=Nx×Ny×Nz, and distribute the task over Pw=Px×Py×

Pzprocessors. If no communication were required, the number of points per processor

would be Nw

=Nx×Ny×Nz

Px×Py×Pz

.(26)

However, for ﬁnite difference codes some communication is required, and the amount of

communication depends on spatial order of the scheme, Q. The PENCIL CODE works by

5.21 Running in double-precision 51

default with sixth order ﬁnite differences, so Q= 6, i.e. one needs 6 ghost zones, 3 on

each end of the mesh. With Q6= 0 the number of points per processor is

N(eﬀ)

=Nx

+Q×Ny

+Q×Nz

+Q.(27)

There is efﬁcient scaling only when

min Nx

,Ny

,Nz

Pz≫Q. (28)

In the special case were Nx=Ny=Nz≡N=N1/3

w, with Px= 1 and Py=Pz≡P=P1/2

we have

N(eﬀ)

= (N+Q)×N

P+Q2

.(29)

For N= 128 and Q= 6 the effective mesh size exceeds the actual mesh size by a factor

N(eﬀ)

= (N+Q)×N

P+Q2

×Pw

.(30)

These factors are listed in Table 3.

Table 3: N(eﬀ)

w/Nwversus Nand P.

P\N128 256 512 1024 2048

1 1.15 1.07 1.04 1.02 1.01

2 1.19 1.09 1.05 1.02 1.01

4 1.25 1.12 1.06 1.03 1.01

8 1.34 1.16 1.08 1.04 1.02

16 1.48 1.22 1.11 1.05 1.03

32 1.68 1.31 1.15 1.07 1.04

64 1.98 1.44 1.21 1.10 1.05

128 2.45 1.64 1.30 1.14 1.07

256 3.21 1.93 1.43 1.20 1.10

512 4.45 2.40 1.62 1.29 1.14

Ideally, one wants to keep the work in the ghost zones at a minimum. If one accepts

that 20–25% of work are done in the ghost zones, one should use 4 processors for 1283

mesh points, 16 processors for 2563mesh points, 64 processors for 5123mesh points, 256

processors for 10243mesh points, and 512 processors for 15363mesh points.

5.21 Running in double-precision

With many compilers, you can easily switch to double precision (8-byte ﬂoating point

numbers) as follows.

Add the lines

# Use double precision

REAL_PRECISION = double

52 THE PENCIL CODE

to ‘src/Makefile.local’ and (re-)run pc_setupsrc.

REAL PRECISION

is set to ‘double’, the ﬂag

FFLAGS DOUBLE

is appended to

the Fortran compile ﬂags. The default for

FFLAGS DOUBLE

is -r8, which works for

g95

or ifort; for

gfortran

, you need to make sure that

FFLAGS DOUBLE

is set to

-fdefault-real-8.

You can see the ﬂags in ‘src/Makefile.inc’, which is the ﬁrst place to check if you have

problems compiling for double precision.

Using double precision might be important in turbulence runs where the resolution

is 2563meshpoints and above (although such runs often seem to work ﬁne at single

precision). To continue working in double precision, you just say lread_from_other_-

prec=T in run_pars; see Sect. F.1.

5.22 Power spectrum

Given a real variable u, its Fourier transform ˜uis given by

˜u(kx, ky, kz) = F(u(x, y, z)) = 1

NxNyNz

Nx−1

p=0

Ny−1

q=0

Nz−1

r=0

u(xp, yq, zr)

×exp(−ikxxp) exp(−ikyyq) exp(−ikzzr),(31)

where

|kx|<πNx

,|ky|<πNy

,|kz|<πNz

when Lis the size of the simulation box. The three-dimensional power spectrum P(k)is

deﬁned as

P(k) = 1

2˜u˜u∗,(32)

where

k=qk2

x+k2

y+k2

z.(33)

Note that we can only reasonably calculate P(k)for k < πNx/Lx.

To get power spectra from the code, edit ‘run.in’ and add for example the following lines

dspec=5., ou_spec=T, ab_spec=T !(for energy spectra)

oned=T

under run_pars. The kinetic (vel_spec) and magnetic (mag_spec) power spectra will

now be calculated every 5.0 (dspec) time units. The Fourier spectra is calculated using

fftpack

. In addition to calculating the three-dimensional power spectra also the one-

dimensional power spectra will be calculated (oned).

In addition one must edit ‘src/Makefile.local’ and add the lines

FOURIER = fourier_fftpack

POWER = power_spectrum

Running the code will now create the ﬁles ‘powerhel_mag.dat’ and ‘power_kin.dat’

containing the three-dimensional magnetic and kinetic power spectra respectively. In

addition to these three-dimensional ﬁles we will also ﬁnd the one-dimensional ﬁles

‘powerbx_x.dat’, ‘powerby_x.dat’, ‘powerbz_x.dat’, ‘powerux_x.dat’, ‘poweruy_x.dat’ and

5.22 Power spectrum 53

‘poweruz_x.dat’. In these ﬁles the data are stored such that the ﬁrst line contains the

time of the snapshot, the following

nxgrid

/2numbers represent the power at each

wavenumber, from the smallest to the largest. If several snapshots have been saved,

they are being stored immediately following the preceding snapshot.

You can read the results with the idl procure ‘power’, like this:

power,’_kin’,’_mag’,k=k,spec1=spec1,spec2=spec2,i=n,tt=t,/noplot

power,’hel_kin’,’hel_mag’,k=k,spec1=spec1h,spec2=spec2h,i=n,tt=t,/noplot

If powerhel is invoked, krms is written during the ﬁrst computation. The relevant out-

put ﬁle is ‘power_krms.dat’. This is needed for a correct calculation of kused in the

realizability conditions.

A caveat of the implementation of Fourier transforms in the PENCIL CODE is that, due

to the parallelization, the permitted resolution is limited to the case when one direction

is an integer multiple of the other. So, it can be done for

Nx = n*Ny

Unfortunately, for some applications one wants Nx < Ny. Wlad experimented with ar-

bitrary resolution by interpolating xto the same resolution of yprior to transposing,

then transform the interpolated array and then interpolating it back (check ‘fourier_-

transform_y’ in ‘fourier_fftpack.f90’).

A feature of our current implementation with xparallelization is that fft_xyz_-

parallel_3D requires nygrid to be an integer multiple of nprocy*nprocz. Examples of

good mesh layouts are listed in Table 4.

Table 4: Examples of mesh layouts for which Fourier transforms with xparallelization is possible.

ny nprocyx nprocy nprocz ncpus

256 1 16 16 256

256 2 16 16 512

256 4 16 16 1024

256 8 16 16 2048

288 2 16 18 576

512 2 16 32 1024

512 4 16 16 1024

512 4 16 32 2048

576 4 18 32 2304

576 8 18 32 4608

576 16 18 32 9216

1024 4 32 32 4096

1024 4 16 64 4096

1024 8 16 32 4096

1152 4 36 32 4608

1152 4 32 36 4608

2304 2 32 72 4608

2304 4 36 64 9216

2304 4 32 72 9216

To visualize with

IDL

just type power and you get the last snapshot of the three-

54 THE PENCIL CODE

dimensional power spectrum. See head of ‘$PENCIL_HOME/idl/power.pro’ for options to

power.

5.23 Structure functions

We deﬁne the p-th order longitudinal structure function of uas

long(l) = h|ux(x+l, y, z)−ux(x, y, z)|pi,(34)

while the transverse is

trans(l) = h|uy(x+l, y, z)−uy(x, y, z)|pi+h|uz(x+l, y, z)−uz(x, y, z)|pi.(35)

Edit ‘run.in’ and add for example the following lines

dspec=2.3,

lsfu=T, lsfb=T, lsfz1=T, lsfz2=T

under run_pars. The velocity (lsfu), magnetic (lsfb) and Elsasser (lsfz1 and lsfz2)

structure functions will now be calculated every 2.3 (dspec) time unit.

In addition one must edit ‘src/Makefile.local’ and add the line

STRUCT_FUNC = struct_func

In ‘src/cparam.local’, deﬁne

lb nxgrid

and make sure that

nxgrid = nygrid = nzgrid = 2**lb_nxgrid

E.g.

integer, parameter :: lb_nxgrid=5

integer, parameter :: nxgrid=2**lb_nxgrid,nygrid=nxgrid,nzgrid=nxgrid

Running the code will now create the ﬁles:

‘sfu-1.dat’, ‘sfu-2.dat’, ‘sfu-3.dat’ (velocity),

‘sfb-1.dat’, ‘sfb-2.dat’, ‘sfb-3.dat’ (magnetic ﬁeld),

‘sfz1-1.dat’, ‘sfz1-2.dat’, ‘sfz1-3.dat’ (ﬁrst Elsasser variable),

‘sfz2-1.dat’, ‘sfz2-2.dat’, ‘sfz2-3.dat’ (second Elsasser variable),

which contains the data of interest. The ﬁrst line in each ﬁle contains the time tand

the number

qmax

, such that the largest moment calculated is

qmax

−1. The next

imax

numbers represent the ﬁrst moment structure function for the ﬁrst snapshot, here

imax

= 2ln(

nxgrid

)

ln 2 −2.(36)

The next

imax

numbers contain the second moment structure function, and so on until

qmax

−1. The following

imax

numbers then contain the data of the signed third order

structure function i.e. S3

long(l) = h[ux(x+l, y, z)−ux(x, y, z)]3i.

The following

imax

qmax

×2numbers are zero if

nr directions

= 1 (default), otherwise

they are the same data as above but for the structure functions calculated in the y and

z directions.

5.24 Particles 55

If the code has been run long enough as to calculate several snapshots, these snapshots

will now follow, being stored in the same way as the ﬁrst snapshot.

To visualize with

IDL

just type structure and you get the time-average of the ﬁrst order

longitudinal structure function (be sure that ‘pencil-runs/forced/idl/’ is in IDL_PATH).

See head of ‘pencil-runs/forced/idl/structure.pro’ for options to structure.

5.24 Particles

The PENCIL CODE has modules for tracer particles and for dust particles (see Sect. 6.16).

The particle modules are chosen by setting the value of the variable PARTICLES in

Makefile.local to either particles_dust or particles_tracers. For the former case

each particle has six degrees of freedom, three positions and three velocities. For the

latter it sufﬁces to have only three position variables as the velocity of the particles are

equal to the instantaneous ﬂuid velocity at that point. In addition one can choose to have

several additional internal degrees of freedoms for the particles. For example one can

temporally evolve the particles radius by setting PARTICLES_RADIUS to particles_radius

in Makefile.local.

All particle infrastructure is controlled and organized by the Particles_main module.

This module is automatically selected by Makefile.src if PARTICLES is different from

noparticles. Particle modules are compiled as a separate library. This way the main

part of the Pencil Code only needs to know about the particles_main.a library, but not

of the individual particle modules.

For a simulation with particles one must in addition deﬁne a few parameters in

cparam.local. Here is a sample of cparam.local for a parallel run with 2,000,000 parti-

cles:

integer, parameter :: ncpus=16, nprocy=4, nprocz=4, nprocx=1

integer, parameter :: nxgrid=128, nygrid=256, nzgrid=128

integer, parameter :: npar=2000000, mpar_loc=400000, npar_mig=1000

integer, parameter :: npar_species=2

The parameter npar is the number of particles in the simulation, mpar_loc is the number

of particles that is allowed on each processor and npar_mig is the number of particles

that are allowed to migrate from one processor to another in any time-step. For a non-

parallel run it is enough to specify npar. The number of particle species is set through

npar_species (assumed to be one if not set). The particle input parameters are given in

start.in and run.in. Here is a sample of the particle part of start.in for dust particles:

&particles_init_pars

initxxp=’gaussian-z’, initvvp=’random’

zp0=0.02, delta_vp0=0.01, eps_dtog=0.01, tausp=0.1

lparticlemesh_tsc=T

The initial positions and velocities of the dust particles are set in initxxp and initvvp.

The next four input parameters are further speciﬁcations of the initial condition. Inter-

action between the particles and the mesh, e.g. through drag force or self-gravity, require

a mapping of the particles on the mesh. The PENCIL CODE currently supports NGP

(Nearest Grid Point, default), CIC (Cloud in Cell, set lparticlemesh_cic=T) and TSC

56 THE PENCIL CODE

(Triangular Shaped Cloud, set lparticlemesh_tsc=T). See Youdin & Johansen (2007) for

details.

Here is a sample of the particle part of run.in (also for dust particles):

&particles_run_pars

ldragforce_gas_par=T

cdtp=0.2

The logical ldragforce_gas_par determines whether the dust particles inﬂuence the gas

with a drag force. cdtp tells the code how many friction times should be resolved in a

minimum time-step.

The sample run ‘samples/sedimentation/’ contains the latest setup for dust particles.

5.24.1 Particles in parallel

The particle variables (e.g. xiand vi) are kept in the arrays fp and dfp. For parallel

runs, particles must be able to move from processor to processor as they pass out of the

(x, y, z)-interval of the local processor. Since not all particles are present at the same

processor at the same time (hopefully), there is some memory optimization in making

fp not big enough to contain all the particles at once. This is achieved by setting the code

variable mpar_loc less than npar in cparam.local for parallel runs. When running with

millions of particles, this trick is necessary to keep the memory need of the code down.

The communication of migrating particles between the processors happens as follows

(see the subroutine redist_particles_procs in particles_sub.f90):

1. In the beginning of each time-step all processors check if any of their particles have

crossed the local (x, y, z)-interval. These particles are called migrating particles. A

run can have a maximum of npar_mig migrating particles in each time-step. The

value of npar_mig must be set in cparam.local. The number should (of course) be

slightly larger than the maximum number of migrating particles at any time-step

during the run. The diagnostic variable nmigmax can be used to output the maxi-

mum number of migrating particles at a given time-step. One can set lmigration_-

redo=T in &particles_run_pars to force the code to redo the migration step if more

than npar_mig want to migrate. This does slow the code down somewhat, but has

the beneﬁt that the code does not stop when more than npar_mig particles want to

migrate.

2. The index number of the receiving processor is then calculated. This requires some

assumption about the grid on other processors and will currently not work for

nonequidistant grids. Particles do not always pass to neighboring processors as the

global boundary conditions may send them to the other side of the global domains

(periodic or shear periodic boundary conditions).

3. The migrating particle information is copied to the end of fp, and the empty spot

left behind is ﬁlled up with the particle of the highest index number currently

present at the processor.

4. Once the number of migrating particles is known, this information is shared with

neighboring processors (including neighbors over periodic boundaries) so that they

5.24 Particles 57

all know how many particles they have to receive and from which processors.

5. The communication happens as directed MPI communication. That means that

processors 0 and 1 can share migrating particles at the same time as processors 2

and 3 do it. The communication happens from a chunk at the end of fp (migrating

particles) to a chunk that is present just after the particle of the highest index

number that is currently at the receiving processor. Thus the particles are put

directly at their ﬁnal destination, and the migrating particle information at the

source processor is simply overwritten by other migrating particles at the next

time-step.

6. Each processor keeps track of the number of particles that it is responsible for. This

number is stored in the variable npar_loc. It must never be larger than mpar_loc

(see above). When a particle leaves a processor, npar_loc is reduced by one, and

then increased by one at the processor that receives that particle. The maximum

number of particles at any processor is stored in the diagnostic variable nparmax. If

this value is not close to npar/ncpus, the particles have piled up in such a way that

computations are not evenly shared between the processors. One can then try to

change the parallelization architecture (nprocy and nprocz) to avoid this problem.

In simulations with many particles (comparable to or more than the number of grid

cells), it is crucial that particles are shared relatively evenly among the processors. One

can as a ﬁrst approach attempt to not parallelize directions with strong particle density

variations. However, this is often not enough, especially if particles clump locally.

Alternatively one can use Particle Block Domain Decomposition (PBDD, see Johansen

et al. 2011). The steps in Particle Block Domain Decomposition scheme are as follows:

1. The ﬁxed mesh points are domain-decomposed in the usual way (with

ncpus=nprocx×nprocy×nprocz).

2. Particles on each processor are counted in bricks of size nbx×nby×nbz (typically

nbx=nby=nbz=4).

3. Bricks are distributed among the processors so that each processor has approxi-

mately the same number of particles

4. Adopted bricks are referred to as blocks.

5. The Pencil Code uses a third order Runge-Kutta time-stepping scheme. In the be-

ginning of each sub-time-step particles are counted in blocks and the block counts

communicated to the bricks on the parent processors. The particle density assigned

to ghost cells is folded across the grid, and the ﬁnal particle density (deﬁned on the

bricks) is communicated back to the adopted blocks. This step is necessary because

the drag force time-step depends on the particle density, and each particle assigns

density not just to the nearest grid point, but also to the neighboring grid points.

6. In the beginning of each sub-time-step the gas density and gas velocity ﬁeld is

communicated from the main grid to the adopted particle blocks.

7. Drag forces are added to particles and back to the gas grid points in the adopted

blocks. This partition aims at load balancing the calculation of drag forces.

8. At the end of each sub-time-step the drag force contribution to the gas velocity ﬁeld

is communicated from the adopted blocks back to the main grid.

58 THE PENCIL CODE

Particle Block Domain Decomposition is activated by setting PARTICLES = particles_-

dust_blocks and PARTICLES_MAP = particles_map_blocks in Makefile.local. A sam-

ple of cparam.local for Particle Block Domain Decomposition can be found in

samples/sedimentation/blocks:

integer, parameter :: ncpus=4, nprocx=2, nprocy=2, nprocz=1

integer, parameter :: nxgrid=32, nygrid=32, nzgrid=32

integer, parameter :: npar=10000, mpar_loc=5000, npar_mig=100

integer, parameter :: npar_species=4

integer, parameter :: nbrickx=4, nbricky=4, nbrickz=4, nblockmax=32

The last line deﬁnes the number of bricks in the total domain – here we divide the grid

into 4×4×4bricks each of size 8×8×8grid points. The parameter nblockmax tells the

code the maximum number of blocks any processor may adopt. This should not be so low

that there is not room for all the bricks with particles, nor so high that the code runs out

of memory.

5.24.2 Large number of particles

When dealing with large number of particles, one needs to make sure that the number

of particles npar is less than the maximum integer that the compiler can handle with.

The maximum integer can be checked by the Fortran intrinsic function huge,

program huge_integers

print *, huge(0_4) ! for default Fortran integer (32 Bit)

print *, huge(0_8) ! for 64 Bit integer in Fortran

end program huge_integers

If the number of particles npar is larger than default maximum integer, one can promote

the maximum integer to 64 Bit by setting

integer(kind=8), parameter :: npar=4294967296

in the cparam.local ﬁle. This works because the data type of npar is only set here. It is

worth noting that one should not use the ﬂag

FFLAGS += -integer-size 64

to promote all the integers to 64 Bit. This will break the Fortran-C interface. One

should also make sure that npar_mig<=npar/ncpus. It is also beneﬁcial to set mpar_-

loc=2*npar/ncpus.

5.24.3 Random number generator

There are several methods to generate random number in the code. It is worth noting

that when simulating coagulation with the super-particle approach, one should use the

intrinsic random number generator of FORTRAN instead of the one implemented in the

code. When invoking random_number_wrapper, there will be back-reaction to the gas ﬂow.

This unexpected back-reaction can be tracked by inspecting the power spectra, which

exhibits the oscillation at the tail. To avoid this, one should set luser_random_number_-

wrapper=F under the module particles_coag_run_pars in run.in.

5.25 Non-cartesian coordinate systems 59

5.25 Non-cartesian coordinate systems

Spherical coordinates are invoked by adding the following line in the ﬁle ‘start.in’

&init_pars

coord_system=’spherical_coords’

One can also invoke cylindrical coordinates by saying cylindrical_coords instead. In

practice, the names (x, y, z)are still used, but they refer then to (r, θ, φ)or (r, φ, z)instead.

When working with curvilinear coordinates it is convenient to use differential operators

in the non-coordinate basis, so the derivatives are taken with respect to length, and

not in a mixed fashion with respect to length for ∂/∂r and with respect to angle for

∂/∂θ and ∂/∂φ. The components in the non-coordinate basis are denoted by hats, see,

e.g., [27], p. 213; see also Appendix B of [28]. For spherical polar coordinates the only

nonvanishing Christoffel symbols (or connection coefﬁcients) are

Γˆ

ˆrˆ

θ= Γˆ

ˆrˆ

φ=−Γˆrˆ

θˆ

θ=−Γˆrˆ

φˆ

φ= 1/r, (37)

Γˆ

φˆ

θˆ

φ=−Γˆ

θˆ

φˆ

φ= cot θ/r. (38)

The Christoffel symbols enter as correction terms for the various differential opera-

tors in addition to a term calculated straightforwardly in the non-coordinate basis. The

derivatives of some relevant Christoffel symbols are

Γˆ

ˆrˆ

θ,ˆ

θ= Γˆ

ˆrˆ

φ, ˆ

φ= Γˆ

φˆ

θˆ

φ, ˆ

φ= 0 (39)

Γˆ

ˆrˆ

θ,ˆr= Γˆ

ˆrˆ

φ,ˆr=−r−2(40)

Γˆ

φˆ

θˆ

φ,ˆ

θ=−r−2sin−2θ(41)

Further details are given in Appendix I.

60 THE PENCIL CODE

6 The equations

The equations solved by the PENCIL CODE are basically the standard compressible

MHD equations. However, the modular structure allows some variations of the MHD

equations, as well as switching off some of the equations or individual terms of the

equation (nomagnetic, noentropy, etc.).

In this section the equations are presented in their most complete form. It may be ex-

pected that the code can evolve most subsets or simpliﬁcations of these equations.

6.1 Continuity equation

In the code the continuity equation, ∂ρ/∂t +∇·ρu= 0, is written in terms of ln ρ,

D ln ρ

Dt=−∇·u.(42)

Here ρdenotes density, uthe ﬂuid velocity, tis time and D/Dt≡∂/∂t +u·∇is the

convective derivative.

6.2 Equation of motion

In the equation of motion, using a perfect gas, the pressure term, can be expressed as

−ρ−1∇p=−c2

s(∇s/cp+∇ln ρ), where the squared sound speed is given by

s=γp

ρ=c2

s0 exp γs/cp+ (γ−1) ln ρ

ρ0,(43)

and γ=cp/cvis the ratio of speciﬁc heats, or adiabatic index. Note that c2

sis proportional

to the temperature with c2

s= (γ−1)cpT.

The equation of motion is accordingly

Dt=−c2

s∇s

+ ln ρ−∇Φgrav +j×B

+ν∇2u+1

3∇∇ ·u+ 2S·∇ln ρ+ζ(∇∇ ·u) ; (44)

Here Φgrav is the gravity potential, jthe electric current density, Bthe magnetic ﬂux

density, νis kinematic viscosity, ζdescribes a bulk viscosity, and, in Cartesian coordi-

nates

Sij =1

2∂ui

∂xj

+∂uj

∂xi−2

3δij∇·u(45)

is the rate-of-shear tensor that is traceless, because it can be written as the generic rate-

of-strain tensor minus its trace. In curvilinear coordinates, we have to replace partial

differentiation by covariant differentiation (indicated by semicolons), so we write Sij =

2(ui;j+uj;i)−1

3δij∇·u.

The interpretation of the two viscosity terms varies greatly depending upon the Viscos-

ity module used, and indeed on the parameters given to the module. See §6.6.

For isothermal hydrodynamics, see §6.4 below.

6.3 Induction equation 61

6.3 Induction equation

∂A

∂t =u×B−ηµ0j.(46)

Here Ais the magnetic vector potential, B=∇ × Athe magnetic ﬂux density, η=

1/(µ0σ)is the magnetic diffusivity (σdenoting the electrical conductivity), and µ0the

magnetic vacuum permeability. This form of the induction equation corresponds to the

Weyl gauge

Φ = 0, where Φdenotes the scalar potential.

6.4 Entropy equation

The current thermodynamics module

entropy

formulates the thermal part of the physics

in terms of entropy s, rather than thermal energy e, which you may be more famil-

iar with. Thus the two fundamental thermodynamical variables are ln ρand s. The

reason for this choice of variables is that entropy is the natural physical variable for

(at least) convection processes: the sign of the entropy gradient determines convective

(in)stability, the Rayleigh number is proportional to the entropy gradient of the associ-

ated hydrostatic reference solution, etc. The equation solved is

ρT Ds

Dt=H − C +∇·(K∇T) + ηµ0j2+ 2ρνS⊗S+ζρ (∇·u)2.(47)

Here, Tis temperature, cpthe speciﬁc heat at constant pressure, Hand Care explicit

heating and cooling terms, Kis the radiative (thermal) conductivity, ζdescribes a bulk

viscosity, and Sis the rate-of-shear tensor that is traceless.

In the entropy module we solve for the speciﬁc entropy, s. The heat conduction term on

the right hand side can be written in the form

∇·(K∇T)

ρT (48)

=cpχh∇2ln T+∇ln T·∇(ln T+ ln χ+ ln ρ)i(49)

=cpχγ∇2s/cp+ (γ−1)∇2ln ρ

+cpχ[γ∇s/cp+ (γ−1)∇ln ρ]·[γ(∇s/cp+∇ln ρ) + ∇ln χ],(50)

where χ=K/(ρcp)is the thermal diffusivity. The latter equation shows that the diffu-

sivity for sis γχ, which is what we have used in Eq. (24).

In an alternative formulation for a constant K, the heat conduction term on the right

hand side can also be written in the form

∇·(K∇T)

ρT =K

ρh∇2ln T+ (∇ln T)2i(51)

which is the form used when constant Kis chosen.

Note that by setting γ= 1 and initially s= 0, one obtains an isothermal equation of

state (albeit at some unnecessary expense of memory). Similarly, by switching off the

evolution terms of entropy, one immediately gets polytropic behavior (if swas initially

constant) or generalized polytropic behavior (where sis not uniform, but ∂s/∂t = 0).

A better way to achieve isothermality is to use the

noentropy

module.

62 THE PENCIL CODE

6.4.1 Viscous heating

We can write the viscosity as the divergence of a tensor τij,j ,

ρ∂ui

∂t =... +τij,j ,(52)

where τij = 2νρSij is the stress tensor. The viscous power density Pis

P=uiτij,j (53)

=∂

∂xj

(uiτij)−ui,j τij (54)

The term under the divergence is the viscous energy ﬂux and the other term is the

kinetic energy loss due to heating. The heating term +ui,jτij is positive deﬁnite, because

τij is a symmetric tensor and the term only gives a contribution from the symmetric part

of ui,j, which is 1

2(ui,j +uj,i), so

ui,jτij =1

2νρ(ui,j +uj,i)(2Sij ).(55)

But, because Sij is traceless, we can add anything proportional to δij and, in particular,

we can write

ui,jτij =1

2(ui,j +uj,i)(2νρSij )(56)

2(ui,j +uj,i −1

3δij∇·u)(2νρSij)(57)

= 2νρS2,(58)

which is positive deﬁnite.

6.4.2 Alternative description

By setting pretend_lnTT=T in init_pars or run_pars (i.e. the general part of the name

list) the logarithmic temperature is used instead of the entropy. This has computational

advantages when heat conduction (proportional to K∇T) is important. Another alterna-

tive is to use another module, i.e. set ENTROPY=temperature_idealgas in ‘Makefile.local’.

When pretend_lnTT=T is set, the entropy equation

∂s

∂t =−u·∇s+1

ρT RHS (59)

is replaced by

∂ln T

∂t =−u·∇ln T+1

ρcvTRHS −(γ−1) ∇·u,(60)

where RHS is the right hand side of equation (47).

6.5 Transport equation for a passive scalar 63

6.5 Transport equation for a passive scalar

In conservative form, the equation for a passive scalar is

∂

∂t(ρc) + ∇·[ρcu−ρD∇c] = 0.(61)

Here cdenotes the concentration (per unit mass) of the passive scalar and Dits diffusion

constant (assumed constant). In the code this equation is solved in terms of ln c,

D ln c

Dt=D∇2ln c+ (∇ln ρ+∇ln c)·∇ln c.(62)

Using ln cinstead of chas the advantage that it enforces c > 0for all times. However,

the disadvantage is that one cannot have c= 0. For this reason we ended up using the

non-logarithmic version by invoking PSCALAR=pscalar_nolog.

6.6 Bulk viscosity

For a monatomic gas it can be shown that the bulk viscosity vanishes. We therefore don’t

use it in most of our runs. However, for supersonic ﬂows, or even otherwise, one might

want to add a shock viscosity which, in its simplest formulation, take the form of a bulk

viscosity.

6.6.1 Shock viscosity

Shock viscosity, as it is used here and also in the Stagger Code of ˚

Ake Nordlund, is

proportional to positive ﬂow convergence, maximum over ﬁve zones, and smoothed to

second order,

ζshock =cshock Dmax

5[(−∇·u)+]E(min(δx, δy, δz))2,(63)

where cshock is a constant deﬁning the strength of the shock viscosity. In the code this

dimensionless coefﬁcient is called nu_shock, and it is usually chosen to be around unity.

Assume that the shock viscosity only enters as a bulk viscosity, so the whole stress

tensor is then

τij = 2ρνSij +ρζshockδij ∇·u.(64)

Assume ν=const, but ζ6=const, so

ρ−1Fvisc =ν∇2u+1

3∇∇ ·u+ 2S·∇ln ρ+ζshock [∇∇ ·u+ (∇ln ρ+∇ln ζshock)∇·u].

(65)

and

ρ−1Γvisc = 2νS2+ζshock(∇·u)2.(66)

In the special case with periodic boundary conditions, we have 2hS2i=hω2i+4

3h(∇·u)2i.

6.7 Equation of state

In its present conﬁguration only hydrogen ionization is explicitly included. Other con-

stituents (currently He and H2) can have ﬁxed values. The pressure is proportional to

the total number of particles, i.e.

p= (nHI +nHII +nH2+ne+nHe +...)kBT. (67)

64 THE PENCIL CODE

It is convenient to normalize to the total number of H both in atomic and in molecular

hydrogen, nHtot ≡nH+ 2nH2, where nHI +nHII =nH, and deﬁne xe≡ne/nHtot,xHe ≡

nHe/nHtot, and xH2≡nH2/nHtot. Substituting nH=nHtot −2nH2, we have

p= (1 −xH2+xe+xHe +...)nHtotkBT. (68)

This can be written in the more familiar form

p=R

µρT, (69)

where R=kB/muand muis the atomic mass unit (which is for all practical purposes the

same as mHtot) and

µ=nH+ 2nH2+ne+ 4nHe

nH+nH2+ne+nHe

=1 + 4xHe

1−xH2+xe+xHe

(70)

is the mean molecular weight (which is here dimensionless; see Kippenhahn & Weigert

1990, p. 102). The factor 4 is really to be substituted for 3.97153. Some of the familiar

relations take still the usual form, in particular e=cvTand h=cpTwith cv=3

2R/µ and

cp=5

2R/µ.

The number ratio, xHe, is more commonly expressed as the mass ratio, Y=

mHenHe/(mHnHtot +mHenHe), or Y= 4xHe/(1 + 4xHe), or 4xHe = (1/Y −1)−1. For exam-

ple, Y= 0.27 corresponds to xHe = 0.092 and Y= 0.25 to xHe = 0.083. Note also that for

100% H2abundance, xH2= 1/2.

In the following, the ionization fraction is given as y=ne/nH, which can be different

from xeif there is H2. Substituting for nHin terms of nHtot yields y=xe/(1 −2xH2).

6.8 Ionization

This part of the code can be invoked by setting EOS=eos_ionization (or EOS=eos_-

temperature_ionization) in the ‘Makefile.local’ ﬁle. The equation of state described

below works for variable ionization, and the entropy offset is different from that used in

Eq. (43), which is now no longer valid. As a replacement, one can use EOS=eos_fixed_-

ionization, where the degree of ionization can be given by hand. Here the normalization

of the entropy is the same as for EOS=eos_ionization. This case is described in more de-

tail below.12

We treat the gas as being composed of partially ionized hydrogen and neutral helium.

These are four different particle species, each of which regarded as a perfect gas.

The ionization fraction y, which gives the ratio of ionized hydrogen to the total amount

of hydrogen nH, is obtained from the Saha equation which, in this case, may be written

1−y=1

nHmekBT

2π~23/2

exp −χH

kBT.(71)

The temperature Tcannot be obtained directly from the PENCIL CODE’s independent

variables ln ρand s, but is itself dependent on y. Hence, the calculation of yessentially

becomes a root ﬁnding problem.

12We omit here the contribution of H2.

6.8 Ionization 65

The entropy of a perfect gas consisting of particles of type iis known from the Sackur-

Tetrode equation

Si=kBNi ln "1

ntot mikBT

2π~23/2#+5

2!.(72)

Here Niis the number of particles of a single species and ntot is the total number density

of all particle species.

In addition to the individual entropies we also have to take the entropy of mixing,

Smix =−NtotkBPipiln pi, into account. Summing up everything, we can get a closed ex-

pression for the speciﬁc entropy sin terms of y,ln ρand T, which may be solved for

Figure 5: Dependence of temperature on entropy for different values of the density.

For given ln ρand swe are then able to calculate the ionization fraction yby ﬁnding the

root of

f(y) = ln "1−y

nHmekBT(y)

2π~23/2#−χH

kBT(y).(73)

In the ionized case, several thermodynamic quantities of the gas become dependent on

the ionization fraction ysuch as its pressure, P= (1+ y+xHe)nHkBT, and its internal

energy, E=3

2(1 + y+xHe)nHkBT+yχH, where xHe gives the ratio of neutral helium to the

total amount of hydrogen. The dependence of temperature on entropy is shown in Fig. 5

for different values of the density.

For further details regarding the procedure of solving for the entropy see Sect. H.6 in

the appendix.

6.8.1 Ambipolar diffusion

Another way of dealing with ionization in the PENCIL CODE is through use of the neu-

trals module. That module solves the coupled equations of neutral and ionized gas, in a

two-ﬂuid model

66 THE PENCIL CODE

∂ρi

∂t =−∇·(ρiui) + G(74)

∂ρn

∂t =−∇·(ρnun)− G (75)

∂(ρiui)

∂t =−∇·(ρiui:ui)−∇pi+pe+B2

2µ0+F(76)

∂(ρnun)

∂t =−∇·(ρnun:un)−∇pn− F (77)

∂A

∂t =ui×B(78)

where the subscripts nand iare for neutral and ionized, respectively. The terms Gand

F, through which the two ﬂuids exchange mass and momentum, are given by

G=ζρn−αρ2

i(79)

F=ζρnun−αρ2

iui+γρiρn(un−ui).(80)

In the above equations, ζis the ionization coefﬁcient, αis the recombination coefﬁcient,

and γthe collisional drag strength. By the time of writing (spring 2009), these three

quantities are supposed constant. The electron pressure peis also assumed equal to the

ion pressure. Only isothermal neutrals are supported so far.

In the code, Eq. (74) and Eq. (76) are solved in ‘density.f90’ and ‘hydro.f90’ respectively.

Equation 75 is solved in ‘neutraldensity.f90’ and Eq. (77) in ‘neutralvelocity.f90’. The

sample ‘1d-test/ambipolar-diffusion’ has the current setup for a two-ﬂuid simulation

with ions and neutrals.

6.9 Combustion

The easiest entry into the subject of simulating combustion is through samples/

0d-tests/chemistry_H2_ignition_rkf or samples/1d-tests/H2_flamespeed. The former

case is studying H2 ignition delay, while the second one is focusing on H2 ﬂame-

speed. If you want to study turbulent premixed ﬂames, the recommended cases are

samples/2d-tests/2d_methane_flame and samples/turbulent_flame. Here, the ﬁrst of

these examples is not really realistic since its only 2D, but this does of course make

it faster to try out. Also, this case is easier to set up. The most realistic test case is

samples/turbulent_flame, which studies a full 3D hydrogen ﬂame. This test case re-

quires that a set of smaller pre-runs are ﬁnalized before the main simulation can be run

(see the associated README ﬁle for more details).

The chemistry_H2_ignition_rkf directory, for example, has the ﬁle ‘tran.dat’, which

contains the parameters characterizing the transport properties, and ‘chem.inp’, which

contains the NASA polynomials; see Eq. (18) of Ref. [2].

6.10 Radiative transfer

Here we only state the basic equations. A full description about the implementation is

given in Sect. H.7 and in the original paper by Heinemann et al. (2006).

6.11 Self-gravity 67

The basic equation for radiative transfer is

dτ =−I+S , (81)

where

τ≡

χ(s′)ds′(82)

is the optical depth (sis the geometrical coordinate along the ray).

Note that radiative transfer is called also in ‘start.csh’, and again each time a snapshot

is being written, provided the output of auxiliary variables is being requested

lwrite -

aux=T

. (Also, of course, the pencil check runs radiative transfer 7 times, unless you put

pencil_check_small=F.)

6.11 Self-gravity

The PENCIL CODE can consider the self-gravity of the ﬂuid in the simulation box by

adding the term

∂u

∂t =...−∇φself (83)

to the equation of motion. The self-potential φself (or just φfor simplicity) satisﬁes Pois-

son’s equation

∇2φ= 4πGρ . (84)

The solution for a single Fourier component at scale kis

φk=−4πGρk

k2.(85)

Here we have assumed periodic boundary conditions. The potential is obtained by

Fourier-transforming the density, then ﬁnding the corresponding potential at that scale,

and ﬁnally Fourier-transforming back to real space.

The x-direction in the shearing sheet is not strictly periodic, but is rather shear periodic

with two connected points at the inner and outer boundary separated by the distance

∆y(t) = mod[(3/2)Ω0Lxt, Ly]in the y-direction. We follow here the method from [18]

to allow for shear-periodic boundaries in the Fourier method for self-gravity. First we

take the Fourier transform along the periodic y-direction. We then shift the entire y-

direction by the amount δy(x) = ∆y(t)x/Lxto make the x-direction periodic. Then we

proceed with Fourier transforms along xand then z. After solving the Poisson equation

in Fourier space, we transform back to real space in the opposite order. We differ here

from the method by [18] in that we shift in Fourier space rather than in real space13.

The Fourier interpolation formula has the advantage over polynomial interpolation in

that it is continuous and smooth in all its derivatives.

6.12 Incompressible and anelastic equations

This part has not yet been documented and is still under development.

13We were kindly made aware of the possibility of interpolating in Fourier space by C. McNally on his

website.

68 THE PENCIL CODE

6.13 Dust equations

The code treats gas and dust as two separate ﬂuids14. The dust and the gas interact

through a drag force. This force can most generally be written as an additional term to

the equation of motion as

Dud

Dt=...−1

τs

(ud−u).(86)

Here τsis the so-called stopping time of the considered dust species. This measures the

coupling strength between dust and gas. In the Epstein drag regime

τs=adρs

csρ,(87)

where adis the radius of the dust grain and ρsis the solid density of the dust grain.

Two other important effects work on the dust. The ﬁrst is coagulation controlled

by the discrete coagulation equation

dnk

dt=1

i+j=k

Aijninj−nk

∞

i=1

Aikni.(88)

In the code Ndiscrete dust species are considered. Also the bins are logarithmically

spaced in order to give better mass resolution. It is also possible to keep track of both

number density and mass density of each bin, corresponding to having a variable grain

mass in each bin.

Dust condensation is controlled by the equation

dt=1

τcond

Nd−1

d.(89)

Here Nis the number of monomers in the dust grain (such as water molecules) and dis

the physical dimension of the dust grain. The condensation time τcond is calculated from

τcond

=A1vthαnmon 1−1

Smon ,(90)

where A1is the surface area of a monomer, αis the condensation efﬁciency, nmon is the

number density of monomers in the gas and Smon is the saturation level of the monomer

given by

Smon =Pmon

Psat

.(91)

Here Psat is the saturated vapor pressure of the monomer. Currently only water ice has

been implemented in the code.

All dust species fulﬁll the continuity equation

∂ρd

∂t +∇·(ρdud) = 0.(92)

14See master’s thesis of A. Johansen (can be downloaded from

http://www.mpia.de/homes/johansen/research_en.php)

6.14 Cosmic ray pressure in diffusion approximation 69

6.14 Cosmic ray pressure in diffusion approximation

Cosmic rays are treated in the diffusion approximation. The equation of state is pc=

(γc)ecwhere the value of γcis usually somewhere between 14/9and 4/3. In the momen-

tum equation (44) the cosmic ray pressure force, −ρ−1∇pcis added on the right hand

side, and ecsatisﬁes the evolution equation

∂ec

∂t +∇·(ecu) + pc∇·u=∂i(Kij ∂jec) + Qc,(93)

where Qcis a source term and

Kij =K⊥δij + (Kk−K⊥)ˆ

Biˆ

Bj(94)

is an anisotropic diffusivity tensor.

In the non-conservative formulation of this code it is advantageous to expand the diffu-

sion term using the product rule, i.e.

∂i(Kij∂jec) = −Uc·∇ec+Kij ∂i∂jec.(95)

where Uci=−∂Kij /∂xjacts like an extra velocity trying to straighten magnetic ﬁeld

lines. We can write this term also as Uc=−(Kk−K⊥)∇·(ˆ

Bˆ

B), where the last term

is a divergence of the dyadic product of unit vectors.15 However, near magnetic nulls,

this term can becomes inﬁnite. In order to avoid this problem we are forced to limit

∇·(ˆ

Bˆ

B), and hence |Uc|, to the maximum possible value that can be resolved at a given

resolution.

A physically appealing way of limiting the maximum propagation speed is to restore

an explicit time dependence in the equation for the cosmic ray ﬂux, and to replace the

diffusion term in Eq. (93) by a divergence of a ﬂux that in turn obeys the equation

∂Fci

∂t =−˜

Kij∇jec−Fci

τ(non-Fickian diffusion),(96)

where Kij =τ˜

Kij would be the original diffusion tensor of Eq. (94), if the time derivative

were negligible. Further details are described in Snodin et al. (2006).

6.15 Chiral MHD

At high energies, kBT&10 MeV, a quantum effect called the chiral magnetic effect (CME)

can modify the MHD equations. The CME occurs in magnetized relativistic plasmas, in

which the number density of left-handed fermions, nL, differs from the one of right-

handed fermions, nR(see e.g., Kharzeev et al. (2013) for a review). This asymmetry is

described by the chiral chemical potential µ5≡6 (nL−nR) (~c)3/(kBT)2, where Tis the

temperature, kBis the Boltzmann constant, cis the speed of light, and ~is the reduced

Planck constant. In the presence of a magnetic ﬁeld, µ5leads to the occurrence of the

current

JCME =αem

π~µ5B,(97)

15In practice, we calculate ∂j(ˆ

Biˆ

Bj) = (δij −2ˆ

Biˆ

Bk)ˆ

BjBk,j /|B|, where derivatives of Bare calculated as

Bi,j =ǫiklAl,jk.

70 THE PENCIL CODE

where αem ≈1/137 is the ﬁne structure constant.

The chiral current (97) adds to the classical Ohmic current, leading to a modiﬁcation of

the Maxwell equations. As a result, the induction equation is extended by one additional

term:

∂A

∂t =U×B−η(∇×B−µB),(98)

where the chiral chemical potential µ5is normalized such that µ= (4αem/~c)µ5. The

latter is determined by the evolution equation

Dµ

Dt =D5∆µ+λ η B·(∇×B)−µB2−Γfµ, (99)

where D5is a chiral diffusion coefﬁcient, λthe chiral feedback parameter, and Γfthe

rate of chiral ﬂipping reactions. All remaining evolution equations are the same as in

classical MHD. Details on the derivation of the chiral MHD equations can be found in

Boyarsky et al. (2015) and Rogachevskii et al. (2017).

In the Pencil Code, the chiral MHD equations can be solved by adding the line

SPECIAL = special/chiral_mhd

to src/Makefile.local. Further, for running the chiral MHD module, one needs to add

&special_init_pars

initspecial=’const’, mu5_const=10.

to start.in and

&special_run_pars

diffmu5=1e-4, lambda5=1e3, cdtchiral=1.0

to run.in, where we have chosen exemplary values for the chiral parameters.

Caution should be taken when solving the chiral MHD equations numerically, since

the evolution of the plasma can be strongly affected by the CME. In particular, the

initial value of µis related to a small-scale dynamo instability. In order to resolve this

instability in a domain of size (2π)3, the minimum number of grid points is given as:

Ngrid &µ0

λ1/22π

νRemesh,crit

.(100)

Also the value of λshould not be chosen too small, since it scales inversely with the

saturation magnetic helicity produced by a chiral dynamo. Hence, for a very small λ

parameter, the Alfv´

en time step becomes extremely small in the non-linear stage which

can lead to a code crash. More details on the numerical modeling of chiral MHD can be

found in Schober et al. (2018).

6.16 Particles

Particles are entities that each have a space coordinate and a velocity vector, where

a ﬂuid only has a velocity vector ﬁeld (the continuity equation of a ﬂuid in some way

corresponds to the space coordinate of particles). In the code particles are present either

as tracer particles or as dust particles

6.16 Particles 71

6.16.1 Tracer particles

Tracer particles always have the local velocity of the gas. The dynamical equations are

thus ∂xi

∂t =u,(101)

where the index iruns over all particles. Here uis the gas velocity at the position of

the particle. One can choose between a ﬁrst order (default) and a second order spline

interpolation scheme (set lquadratic_interpolation=T in &particles_init_pars) to cal-

culate the gas velocity at the position of a tracer particle.

The sample run ‘samples/dust-vortex’ contains the latest setup for tracer particles.

6.16.2 Dust particles

Dust particles are allowed to have a velocity that is not similar to the gas,

dxi

dt=vi.(102)

The particle velocity follows an equation of motion similar to a ﬂuid, only there is no

advection term. Dust particles also experience a drag force from the gas (proportional to

the velocity difference between a particle and the gas).

dvi

dt=...−1

τs

(vi−u).(103)

Here τsis the stopping time of the dust particle. The interpolation of the gas velocity to

the position of a particle is done using one of three possible particle-mesh schemes,

•NGP (Nearest Grid Point, default)

The gas velocity at the nearest grid point is used.

•CIC (Cloud in Cell, set lparticlemesh_cic=T)

A ﬁrst order interpolation is used to obtain the gas velocity ﬁeld at the position of

a particle. Affects 8 grid points.

•TSC (Triangular Shaped Cloud, set lparticlemesh_tsc=T)

A second order spline interpolation is used to obtain the gas velocity ﬁeld at the

position of a particle. Affects 27 grid points.

The particle description is the proper description of dust grains, since they do not feel

any pressure forces (too low number density). Thus there is no guarantee that the grains

present within a given volume will be equilibrated with each other, although drag force

may work for small grains to achieve that. Larger grains (meter-sized in protoplanetary

discs) must be treated as individual particles.

To conserve momentum the dust particles must affect the gas with a friction force as

well. The strength of this force depends on the dust-to-gas ratio ǫd, and it can be safely

ignored when there is much more gas than there is dust, e.g. when ǫd= 0.01. The friction

force on the gas appears in the equation of motion as

∂u

∂t =...−ρ(i)

ρ∂v(i)

∂t drag

(104)

72 THE PENCIL CODE

Here ρ(i)

pis the dust density that particle irepresents. This can be set through the pa-

rameter eps_todt in &particle_init_pars. The drag force is assigned from the particles

onto the mesh using either NGP, CIC or TSC assignment. The same scheme is used both

for interpolation and for assignment to avoid any risk of a particle accelerating itself (see

Hockney & Eastwood 1981).

6.17 N-body solver

The N-body code takes advantage of the existing Particles module, which was coded with

the initial intent of treating solid particles whose radius a•is comparable to the mean

free path λof the gas, for which a ﬂuid description is not valid. A N-body implementation

based on that module only needed to include mass as extra state for the particles, solve

for the N2gravitational pair interactions and distinguish between the N-body and the

small bodies that are mapped into the grid as a ρpdensity ﬁeld.

The particles of the N-body ensemble evolve due to their mutual gravity and by inter-

acting with the gas and the swarm of small bodies. The equation of motion for particle i

dvpi

dt =Fgi−

j6=i

GMj

Rij (105)

where Rij =|rpi−rpj|is the distance between particles iand j, and ˆ

Rij is the unit vector

pointing from particle jto particle i. The ﬁrst term of the R.H.S. is the combined gravity

of the gas and of the dust particles onto the particle i, solved via

Fgi=−GZV

[ρg(r) + ρp(r)]Ri

(R2

i+b2

i)3/2dV, (106)

where the integration is carried out over the whole disk. The smoothing distance biis

taken to be as small as possible (a few grid cells). For few particles (<10), calculating the

integral for every particle is practical. For larger ensembles one would prefer to solve

the Poisson equation to calculate their combined gravitational potential.

The evolution of the particles is done with the same third-order Runge-Kutta time-

stepping routine used for the gas. The particles deﬁne the timestep also by the Courant

condition that they should not move more than one cell at a time. For pure particle runs,

where the grid is absent, one can adopt a ﬁxed time-step tp≪2πΩ−1

fp where Ωfp is the

angular frequency of the fastest particle.

By now (spring 2009), no inertial accelerations are included in the N-body module, so

only the inertial frame - with origin at the barycenter of the N-body ensemble - is avail-

able. For a simulation of the circular restricted three-body problem with mass ratio

q=10−3, the Jacobi constant of a test particle initially placed at position (x, y)=(2,0) was

found to be conserved up to one part in 105within the time span of 100 orbits.

We stress that the level of conservation is poor when compared to integrators designed

to speciﬁcally deal with long-term N-body problems. These integrators are usually sym-

plectic, unlike the Runge-Kutta scheme of the PENCIL CODE. As such, PENCIL should

not be used to deal with evolution over millions of years. But for the time-span typical

of astrophysical hydrodynamical simulations, this degree of conservation of the Jacobi

constant can be deemed acceptable.

6.18 Test-ﬁeld equations 73

Table 5: Scale factor and conformal Hubble parameter for different values of n.

n a HH

0 1 0 0

1/2η/2 1/η 1/η

2/3η2/3 2/η 6/η2

As an extension of the particle’s module, the N-body is fully compatible with the par-

allel optimization of PENCIL, which further speeds up the calculations. Parallelization,

however, is not yet possible for pure particle runs, since it relies on splitting the grid

between the processors. At the time of writing (spring 2009), the N-body code does not

allow the particles to have a time-evolving mass.

6.18 Test-ﬁeld equations

The test-ﬁeld method is used to calculate turbulent transport coefﬁcients for magneto-

hydrodynamics. This is a rapidly evolving ﬁeld and we refer the interested reader to

recent papers in this ﬁeld, e.g. by Sur et al. (2008) or Brandenburg et al. (2008). For

technical details; see also Sect. F.3.

6.19 Gravitational wave equations

The expansion of the universe with time is described by the scale factor a(τ), where τ

is the physical time. Using conformal time, t(τ) = Rτ

0dτ′/a(τ′), and dependent variables

that are appropriately scaled with powers of a, the hydromagnetic equations can be

expressed completely without scale factor [10, 17]. This is not true, however, for the

gravitational wave (GW) equations, where a dependence on aremains [17]. The time

dependence of acan be modeled as a power law, a∝τn, where n= 1/2applies to the

radiation-dominated era; see Table 5 the general relationship. To compare with cases

where the expansion is ignored, we put n= 0.

In the transverse traceless (TT) gauge, the six components of the spatial part of the

symmetric tensor characterizing the linearized evolution of the metric perturbations

hij, reduce to two components which, in the linear polarization basis, are the +and

×polarizations. However, the projection onto that basis is computationally intensive,

because it requires nonlocal operations involving Fourier transformations. It is therefore

advantageous to evolve instead the perturbation of the metric tensor, hij , in an arbitrary

gauge, compute then hTT

ij in the TT gauge, and perform then the decomposition into the

linear polarization basis whenever we compute diagnostic quantities such as averages

or spectra. Thus, we solve the linearized GW equation in the form [17]

∂2hij

∂t2=−2H∂hij

∂t +c2∇2hij +16πG

a2c2Tij (107)

for the six components 1≤i≤j≤3, where tis comoving time, ais the scale factor,

H= ˙a/a is the comoving Hubble parameter, Tij is the source term, cis the speed of light,

and Gis Newton’s constant. For n= 0, when the cosmic expansion is ignored, we have

74 THE PENCIL CODE

a= 1 and H= 0. In practice, we solve the GW equation for the scaled variable ˜

hij =ahij,

∂2˜

hij

∂t2=c2∇2˜

hij +16πG

ac2Tij.(108)

For the numerical treatment of Eq. (108) and equations (110)–(112).

The source term is chosen to be the traceless part of the stress tensor,

Tij(x, t) = ρuiuj−BiBj−1

3δij(ρu2−B2).(109)

The removal of the trace is in principle not necessary, but it helps preventing a contin-

uous build-up of a large trace, which would be numerically disadvantageous. We have

ignored here the viscous stress, which is usually small.

We compute Tij by solving the energy, momentum, and induction equations for an ultra-

relativistic gas in the form [10, 12]

∂ln ρ

∂t =−4

3(∇·u+u·∇ln ρ) + 1

ρu·(J×B) + ηJ2,(110)

Dt =u

3(∇·u+u·∇ln ρ)−u

ρu·(J×B) + ηJ2

−1

4∇ln ρ+3

4ρJ×B+2

ρ∇·(ρνS) + f,(111)

∂B

∂t =∇ × (u×B−ηJ),(112)

where B=∇×Ais the magnetic ﬁeld expressed in terms of the magnetic vector poten-

tial to ensure that ∇·B= 0,J=∇×Bis the current density, D/Dt = ∂/∂t + u ·∇is

the advective derivative, Sij =1

2(ui,j +uj,i)−1

3δijuk,k is the trace-free rate of strain tensor,

and p=ρc2

sis the pressure, where cs=c/√3is the sound speed for an ultra-relativistic

gas. Lorentz-Heaviside units for the magnetic ﬁeld are used.

We are interested in the rms value of the metric tensor perturbations and the GW energy

density in the linear polarization basis. To compute hTT

ij from hij, we Fourier transform

the six components of hij and ˙

hij,

hij(k, t) = Zhij (x, t)e−ik·vd3xfor 1≤i≤j≤3(113)

and compute the components in the TT gauge as

hTT

ij (k, t) = (PilPjm −1

2PijPlm)˜

hlm(k, t),(114)

where Pij =δij −ˆ

kiˆ

kjis the projection operator, and ˆ

k=k/k is the unit vector of k, with

k=|k|being the modulus. Next, we compute the linear polarization bases

ij =e1

ie1

j−e2

ie2

j, e×

ij =e1

ie2

j+e2

ie1

j,(115)

where e1and e2are unit vectors perpendicular to k. Thus

h+(k, t) = 1

2e+

ij(k)˜

hij(k, t),(116)

h×(k, t) = 1

2e×

ij(k)˜

hij(k, t).(117)

6.19 Gravitational wave equations 75

We then return into real space and compute

h+/×(x, t) = Z˜

h+/×(k, t)eik·xd3k/(2π)3.(118)

Analogous calculations are performed for ˙

h+/×(x, t), which are used to compute the GW

energy via

EGW(t) = c2

32πG h˙

+i+h˙

×i,(119)

where angle brackets denote volume averages.

Analogously to kinetic and magnetic energy and helicity spectra, it is convenient to

compute the GW energy and polarization spectra integrated over concentric shells of

surface R4πk2dΩkin kspace, deﬁned by

S˙

h(k) = Z4π|˙

h+|2+|˙

h×|2k2dΩk,(120)

A˙

h(k) = Z4π

2Im ˙

h+˙

h×

∗k2dΩk,(121)

and normalized such that R∞

0S˙

h(k) dk=h˙

+i+h˙

×iis proportional to the energy density

and R∞

0A˙

h(k) dkis proportional to the polarized energy density. The A˙

h(k)spectra are

not to be confused with the magnetic vector potential A(x, t). The corresponding GW

energy spectra are noted by

EGW(k) = (c2/32πG)S˙

h(k),(122)

HGW(k) = (c2/32πG)A˙

h(k).(123)

We also deﬁne spectra for the metric tensor perturbation,

Sh(k) = Z4π|˜

h+|2+|˜

h×|2k2dΩk,(124)

Ah(k) = Z4π

2Im ˜

h+˜

h×

∗k2dΩk,(125)

which are normalized such that R∞

0Sh(k) dk=h2

rms is the mean squared metric tensor

perturbation.

76 THE PENCIL CODE

7 Troubleshooting / Frequently Asked Questions

7.1 Download and setup

7.1.1 Download forbidden

A: Both GitHub and SourceForge are banned from countries on the United

States Ofﬁce of Foreign Assets Control sanction list, including Cuba, Iran, Libya,

North Korea, Sudan and Syria; see http://de.wikipedia.org/wiki/GitHub and

http://en.wikipedia.org/wiki/SourceForge. As a remedy, you might download a tar-

ball from http://pencil-code.nordita.org/; see also Section 2.

7.1.2 When sourcing the ‘sourceme.sh’/‘sourceme.csh’ ﬁle or running pc_setupsrc, I get

error messages from the shell, like ‘if: Expression Syntax.’ or ‘set: Variable name

must begin with a letter.’

A: This sounds like a buggy shell setup, either by yourself or your system administrator

— or a shell that is even more idiosyncratic than the ones we have been working with.

To better diagnose the problem, collect the following information before ﬁling a bug

report to us:

1. uname -a

2. /bin/csh -v

3. echo $version

4. echo $SHELL

5. ps -p $$

6. If you have problems while sourcing the ‘sourceme’ script,

(a) unset the PENCIL_HOME variable:

for

csh

and similar: unsetenv PENCIL_HOME

for

bash

and similar: unexport PENCIL_HOME; unset PENCIL_HOME

(b) switch your shell in verbose mode,

for

csh

and similar: set verbose; set echo

for

bash

and similar: set -v; set -x

then source again.

7. If you have problems with pc_setupsrc, run it with csh in verbose mode:

/bin/csh -v -x $PENCIL_HOME/bin/pc_setupsrc

7.2 Compilation 77

7.2 Compilation

7.2.1 Linker can’t ﬁnd the syscalls functions:

ld: 0711-317 ERROR: Undefined symbol: .is_nan_c

ld: 0711-317 ERROR: Undefined symbol: .sizeof_real_c

ld: 0711-317 ERROR: Undefined symbol: .system_c

ld: 0711-317 ERROR: Undefined symbol: .get_env_var_c

ld: 0711-317 ERROR: Undefined symbol: .get_pid_c

ld: 0711-317 ERROR: Undefined symbol: .file_size_c

A: The Pencil Code needs a working combination of a Fortran- and a C-compiler. If this

is not correctly set up, usually the linker won’t ﬁnd the functions inside the

syscalls

module. If that happens, either the combination of C- and Fortran-compiler is inappro-

priate (e.g.

ifort

needs

icc

), or the compiler needs additional ﬂags, like

g95

might need

the option ‘-fno-second-underscore’ and

xlf

might need the option ‘-qextname’. Please

refer to Sect. 5.2, Table 1.

7.2.2 Make gives the following error now:

PGF90-S-0017-Unable to open include file: chemistry.h (nochemistry.f90: 43)

0 inform, 0 warnings, 1 severes, 0 fatal for chemistry

Line 43 of the nochemistry routine, only has ’contains’.

A: This is because somebody added a new module (together with a corresponding

nomod-

ule.f90

and a

module.h

ﬁle (chemistry in this case). These ﬁles didn’t exist before, so you

need to say:

pc_setupsrc

If this does not help, say ﬁrst make clean and then pc_setupsrc.

7.2.3 How do I compile the PENCIL CODE with the Intel (

ifc

) compiler under

Linux

A: The PENCIL CODE should compile successfully with

ifc

6.x,

ifc

7.0, sufﬁciently recent

versions of

ifc

7.1 (you should get the latest version; if yours is too old, you will typically

get an ‘internal compiler error’ during compilation of ‘src/hydro.f90’), as well as with

recent versions of

ifort

8.1 (8.0 may also work).

You can ﬁnd the

ifort

compiler at ftp://download.intel.com/software/products/compilers/downlo

On many current (as of November 2003) Linux systems, there is a mismatch between

the

glibc

versions used by the compiler and the linker. To work around this, use the

following ﬂag for compiling

FC=ifc -i_dynamic

and set the environment variable

LD_ASSUME_KERNEL=2.4.1; export LD_ASSUME_KERNEL

78 THE PENCIL CODE

setenv LD_ASSUME_KERNEL 2.4.1

This has solved the problems e.g. on a system with glibc-2.3.2 and kernel 2.4.22.

Thanks to Leonardo J. Milano (http://udel.edu/~lmilano/) for part of this info.

7.2.4 I keep getting segmentation faults with ‘start.x’ when compiling with

ifort

8.0

A: There was/is a number of issues with

ifort

8.0. Make sure you have the latest patches

applied to the compiler. A number of things to consider or try are:

1. Compile with the the ‘-static -nothreads’ ﬂags.

2. Set your stacksize to a large value (but a far too large value may be problematic,

too), e. g.

limit stacksize 256m

ulimit -s 256000

3. Set the environment variable KMP STACKSIZE to a large value (like 100M)

See also http://softwareforums.intel.com/ids/board/message?board.id=11&message.id=1375

7.2.5 When compiling with MPI on a Linux system, the linker complains:

mpicomm.o: In function ‘mpicomm_mpicomm_init_’:

mpicomm.o(.text+0x36): undefined reference to ‘mpi_init_’

mpicomm.o(.text+0x55): undefined reference to ‘mpi_comm_size_’

mpicomm.o(.text+0x6f): undefined reference to ‘mpi_comm_rank_’

[...]

A: This is the infamous

underscore problem

. Your

MPI

libraries have been compiled

with

G77

without the option ‘-fno-second-underscore’, which makes the

MPI

symbol

names incompatible with other Fortran compilers.

As a workaround, use

MPICOMM = mpicomm_

in ‘Makefile.local’. Or, even better, you can set this globally (for the given computer)

by inserting that line into the ﬁle ‘~/.adapt-mkfile.inc’ (see perldoc adapt-mkfile for

more details).

7.2.6 Compilation stops with the cryptic error message:

f95 -O3 -u -c .f90.f90

Error : Could not open sourcefile .f90.f90

compilation aborted for .f90.f90 (code 1)

make[1]: *** [.f90.o] Error 1

What is the problem?

A: There are two possibilities:

7.2 Compilation 79

1. One of the variables for

make

has not been set, so

make

expands it to the empty

string. Most probably you forgot to specify a module in ‘src/Makefile.local’. One

possibility is that you have upgraded from an older version of the code that did not

have some of the modules the new version has.

Compare your ‘src/Makefile.local’ to one of the examples that work.

2. One of the variables for

make

has a space appended to it, e.g. if you use the line

MPICOMM = mpicomm_

(see §7.2.5) with a trailing blank, you will encounter this error message. Remove

the blank. This problem can also occur if you added a new module (and have an

empty space after the module name in ‘src/Makefile.src’, i.e.

CHIRAL=nochiral

in which case the compiler will talk about “circular dependence” for the ﬁle

‘nochiral’.

7.2.7 The code doesn’t compile,

. . . there is a problem with

mvar

make start.x run.x

f95 -O3 -u -c cdata.f90

Error: cdata.f90, line 71: Implicit type for MVAR

detected at MVAR@)

[f95 terminated - errors found by pass 1]

make[1]: *** [cdata.o] Error 2

A: Check and make sure that ‘mkcparam’ (directory ‘$PENCIL_HOME/bin’) is in your path. If

this doesn’t help, there may be an empty ‘cparam.inc’ ﬁle in your ‘src’ directory. Remove

‘cparam.inc’ and try again (Note that ‘cparam.inc’ is automatically generated from the

‘Makefile’).

7.2.8 Some samples don’t even compile,

as you can see on the web, http://www.nordita.org/software/pencil-code/tests.html.

samples/helical-MHDturb:

Compiling.. not ok:

make start.x run.x read_videofiles.x

make[1]: Entering directory ‘/home/dobler/f90/pencil-code/samples/helical-MHDturb/src’

/usr/lib/lam/bin/mpif95 -O3 -c initcond.f90

/usr/lib/lam/bin/mpif95 -O3 -c density.f90

use Gravity, only: gravz, nu_epicycle

Error 208 at (467:density.f90) : No such entity in the module

Error 355 : In procedure INIT_LNRHO variable NU_EPICYCLE has not been given a type

Error 355 : In procedure POLYTROPIC_LNRHO_DISC variable NU_EPICYCLE has not been given

3 Errors

compilation aborted for density.f90 (code 1)

make[1]: *** [density.o] Error 1

80 THE PENCIL CODE

make[1]: Leaving directory ‘/home/dobler/f90/pencil-code/samples/helical-MHDturb/src’

make: *** [code] Error 2

A: Somebody may have checked in something without having run auto-test beforehand.

The problem here is that something has been added in one module, but not in the corre-

sponding no-module. You can of course check with

svn

who it was. . .

7.2.9 Internal compiler error with Compaq/Dec F90

The Dec Fortran optimizer has occasional problems with ‘nompicomm.f90’:

make start.x run.x read_videofiles.x

f90 -fast -O3 -tune ev6 -arch ev6 -c cparam.f90

[...]

f90 -fast -O3 -tune ev6 -arch ev6 -c nompicomm.f90

otal vm 2755568 otal vm 2765296 otal vm 2775024

otal vm 2784752 otal...

Assertion failure: Compiler internal error - please submit problem r...

GEM ASSERTION, Compiler internal error - please submit problem report

Fatal error in: /usr/lib/cmplrs/fort90_540/decfort90 Terminated

*** Exit 3

Stop.

*** Exit 1

Stop.

A: The occurrence of this problem depends upon the grid size; and the problem never

seems to occur with ‘mpicomm.f90’, except when ncpus=1. The problem can be avoided by

switching off the loop transformation optimization (part of the ‘-O3’ optimization), via:

#OPTFLAGS=-fast -O3 -notransform_loops

This is currently the default compiler setting in ‘Makefile’, although it has a measurable

performance impact (some 8% slowdown).

7.2.10 Assertion failure under SunOS

Under SunOS, I get an error message like

user@sun> f90 -c param_io.f90

Assertion failed: at_handle_table[at_idx].tag == VAR_TAG,

file ../srcfw/FWcvrt.c, line 4018

f90: Fatal error in f90comp: Abort

A: This is a compiler bug that we ﬁnd at least with Sun’s WorkShop Compiler version ‘5.0

00/05/17 FORTRAN 90 2.0 Patch 107356-05’. Upgrade the compiler version (and possi-

bly also the operating system): we ﬁnd that the code compiles and works with version

‘Sun WorkShop 6 update 2 Fortran 95 6.2 Patch 111690-05 2002/01/17’ under SunOS

version ‘5.8 Generic 108528-11’.

7.2 Compilation 81

7.2.11 After some dirty tricks I got pencil code to compile with MPI, ...

> Before that i installed lam-7.1.4 from source.

Goodness gracious me, you shouldn’t have to compile your own MPI library.

A: Then don’t use the old LAM-MPI. It is long superseded by open-mpi now. Open-mpi

doesn’t need a daemon to be running. I am using the version that ships with Ubuntu

(e.g. 9.04):

frenesi:~> aptitude -w 210 search openmpi | grep ’^i’

i libopenmpi-dev - high performance message passing library -- header files

i A libopenmpi1 - high performance message passing library -- shared library

i openmpi-bin - high performance message passing library -- binaries

i A openmpi-common - high performance message passing library -- common files

i openmpi-doc - high performance message passing library -- man pages

Install that and keep your conﬁguration (Makeﬁle.src and getconf.csh) close to that for

‘frenesi’ or ‘norlx50’. That should work.

7.2.12 Error: Symbol ’mpi comm world’ at (1) has no IMPLICIT type

I installed the pencil code on Ubuntu system and tested "run.csh"

in ...\samples\conv-slab. Here the code worked pretty well.

Nevertheless, running (auto-test), I found there are some errors.

The messages are,

Error: Symbol ’mpi_comm_world’ at (1) has no IMPLICIT type

Fatal Error: Error count reached limit of 25.

make[2]: *** [mpicomm_double.o] Error 1

make[2]: Leaving directory

‘/home/pkiwan/Desktop/pencil-code/samples/2d-tests/selfgravitating-shearwave/src’

make[1]: *** [code] Error 2

make[1]: Leaving directory

‘/home/pkiwan/Desktop/pencil-code/samples/2d-tests/selfgravitating-shearwave/src’

make: *** [default] Error 2

Finally, ### auto-test failed ###

Will it be OK? Or, how can I fix this?

A: Thanks for letting me know about the status, and congratulations on your progress!

Those tests that fail are those that use MPI. If your machine is a dual or multi core

machine, you could run faster by running under MPI. But this is probably not crucial

for you at this point. (I just noticed that there is a ToDo listed in the auto-test command

to implement the option not to run the MPI tests, but this hasn’t been done yet. So I

guess you can start with the science next.

82 THE PENCIL CODE

7.2.13 Error: Can’t open included ﬁle ’mpif.h’

It always worked, but now, after some systems upgrade, I get

gfortran -O3 -o mpicomm.o -c mpicomm.f90

Error: Can’t open included file ’mpif.h’

When I say locate mpif.h I only get things like

/scratch/ntest/1.2.7p1-intel/include/mpif.h

But since I use

FC=mpif90

I thought I don’t need to worry.

A: Since you use

FC=mpif90

there must deﬁnitely be something wrong with their setup.

Try mpif90 -showme or mpif90 -show; the ‘-I’ option should say where it looks for ’mpif.h’.

If those directories don’t exist, it’s no wonder that it doesn’t work, and it is time to

complain.

7.3 Pencil check

7.3.1 The pencil check complains for no reason.

A: The pencil check only complains for a reason.

7.3.2 The pencil check reports MISSING PENCILS and quits

A: This could point to a serious problem in the code. Check where the missing pencil

is used in the code. Request the right pencils, likely based on input parameters, by

adapting one or more of the pencil_criteria_MODULE subroutines.

7.3.3 The pencil check reports unnecessary pencils

The pencil check reports possible overcalculation... pencil rho ( 43) is

requested, but does not appear to be required!

A: Such warnings show that your simulation is possibly running too slowly because it is

calculating pencils that are not actually needed. Check in the code where the unneces-

sary pencils are used and adapt one or more of the pencil_criteria_MODULE subroutines

to request pencils only when they are actually needed.

7.3.4 The pencil check reports that most or all pencils are missing

A: This is typically a thing that can happen when testing new code development for the

ﬁrst time. It is usually an indication that the reference df changes every time you call

pde. Check whether any newly implemented subroutines or functionality has a “mem-

ory”, i.e. if calling the subroutine twice with the same fgives different output df.

7.4 Running 83

7.3.5 Running the pencil check triggers mathematical errors in the code

A: The pencil check puts random numbers in fbefore checking the dependence of df on

the chosen set of pencils. Sometimes these random numbers are inconsistent with the

physics and cause errors. In that case you can set lrandom_f_pencil_check=F in &run_-

pars in ‘run.in’. The initial condition may contain many idealized states (zeros or ones)

which then do not trigger pencil check errors when lrandom_f_pencil_check=F, even if

pencils are missing. But it does prevent mathematical inconsistencies.

7.3.6 The pencil check still complains

A: Then you need to look into the how the code and the pencil check operate. Reduce the

problem in size and dimensions to ﬁnd the smallest problem that makes the pencil check

fail (e.g. 1x1x8 grid points). At the line of ‘pencil_check.f90’ when a difference is found

between df_ref and df, add some debug lines telling you which variable is inconsistent

and in what place. Often you will be surprised that the pencil check has correctly found

a problem in the simulation.

7.3.7 The pencil check is annoying so I turned it off

A: Then you are taking a major risk. If one or more pencils are not calculated properly,

then the results will be wrong.

7.4 Running

7.4.1 Why does ‘start.x’ / ‘start.csh’ write data with periodic boundary conditions?

A: Because you are setting the boundary conditions in ‘run.in’, not in ‘start.in’; see

Sect. 5.16.1. There is nothing wrong with the initial data — the ghost-zone values will

be re-calculated during the very ﬁrst time step.

7.4.2 csh problem?

Q: On some rare occasions we have problems with csh not being supported on other

machines. (We hope to ﬁx this by contacting the responsible person, but may not be that

trivial today!) Oliver says this is a well known bug of some years ago, etc. But maybe in

the long run it would be good to avoid csh.

A: These occasions will become increasingly frequent, and eventually for some architec-

tures, there may not even be a csh variant that can be installed.

We never pushed people to use pc_run and friends (and to report corresponding bugs

and get them ﬁxed), but if we don’t spend a bit of effort (or annoy users) now, we create

a future emergency, where someone needs to run on some machine, but there is no csh

and he or she just gets stuck.

We don’t have that many csh ﬁles, and for years now it should be possible to compile

run without csh (using bin/pc_run) — except that people still fall back on the old way of

84 THE PENCIL CODE

doing things. This is both cause and consequence of the ‘new’ way not being tested that

much, at least for the corner cases like ‘RERUN’, ‘NEWDIR’, ‘SCRATCH_DIR’.

7.4.3 ‘run.csh’ doesn’t work:

Invalid character ’’’ in NAMELIST input

Program terminated by fatal I/O error

Abort

A: The string array for the boundary condition, e.g.

bcx

bcz

is too long. Make sure it

has exactly as many elements as

nvar

is big.

7.4.4 Code crashes after restarting

> > removing mu_r from the namelist just ‘like that’ makes the code

> > backwards incompatible.

> That means that we can never get rid of a parameter in start.in once we

> have introduced it, right?

A: In the current implementation, without a corresponding cleaning procedure, unfor-

tunately yes.

Of course, this does not affect users’ private changes outside the central svn tree.

7.4.5 auto-test gone mad...?

Q: Have you ever seen this before:

giga01:/home/pg/n7026413/cvs-src/pencil-code/samples/conv-slab> auto-test

/home/pg/n7026413/cvs-src/pencil-code/samples/conv-slab:

Compiling.. ok

No data directory; generating data -> /var/tmp/pencil-tmp-25318

Starting.. ok

Running.. ok

Validating results..Malformed UTF-8 character (unexpected continuation

byte 0x80, with no preceding start byte) in split at

/home/pg/n7026413/cvs-src/pencil-code/bin/auto-test line 263.

Malformed UTF-8 character (unexpected continuation byte 0x80, with no

preceding start byte) in split at

/home/pg/n7026413/cvs-src/pencil-code/bin/auto-test line 263.

A: You are running on a RedHat 8 or 9 system, right?

Set

LANG=POSIX

in your shell’s startup script and life will be much better.

7.4 Running 85

7.4.6 Can I restart with a different number of cpus?

Q: I am running a simulation of nonhelical turbulence on the cluster using MPI. Suppose

if I am running a 1283simulation on 32 cpus/cores i.e.

integer, parameter :: ncpus=32,nprocy=2,nprocz=ncpus/nprocy,nprocx=1

integer, parameter :: nxgrid=128,nygrid=nxgrid,nzgrid=nxgrid

And I stop the run after a bit. Is there a way to resume this run with different number

of cpus like this :

integer, parameter :: ncpus=16,nprocy=2,nprocz=ncpus/nprocy,nprocx=1

integer, parameter :: nxgrid=128,nygrid=nxgrid,nzgrid=nxgrid

I understand it has to be so in a new directory but making sure that the run starts from

where I left it off in the previous directory.

A: The answer is no, if you use the standard distributed io. There is also parallel io, but

I never used it. That would write the data in a single ﬁle, and then you could use the

data for restart in another processor layout.

7.4.7 Can I restart with a different number of cpus?

Q: Is it right that once the simulation is resumed, pencil-code takes the last data from

var.dat (which is the current snapshot of the ﬁelds)? If that is true, then, is it not possible

to give that as the initial condition for the run in the second directory (with changed

”ncpus”)? Is there a mechanism already in place for that?

A: Yes, the code restarts from the last var.dat. It is written after a successful completion

of the run, but it crashes or you hit a time-out, there will be a var.dat that is overwritten

every isave timesteps. If the system stops during writing, some var.dat ﬁles may be

corrupt or have the wrong time. In that case you could restart from a good VAR ﬁle, if

you have one, using, e.g.,

restart-new-dir-VAR . 46

where 46 is the number of your VAR ﬁle, i.e., VAR46 im this case. To restart in another

directory, you say, from the old run directory,

restart-new-dir ../another_directory

Hope this helps. Look into pencil-code/bin/restart-new-dir to see what it is doing.

7.4.8 fft xyz parallel 3D: nygrid needs to be an integer multiple...

Q: I just got an:

fft_xyz_parallel_3D: nygrid needs to be an integer multiple of nprocy*nprocz

In my case, nygrid=2048, nprocy=32, and nprocz=128, so nprocy*nprocz=4096. In other

words, 2048 needs to be a multiple of 4096. But isn’t this the case then?

A: No, because 2048 = 0.5 * 4096 and 0.5 is not an integer. Maybe try either setting

nprocz=64 or nprocy=64. You could compensate the change of ncpus with the x-direction.

86 THE PENCIL CODE

For 20483simulations, nprocy=32 and nprocz=64 would be good. A list of good meshes is

given in Table 4.

7.4.9 Unit-agnostic calculations?

Q: The manual speaks about unit-agnostic calculations, stating that one may choose to

interpret the results in any (consistent) units, depending on the problem that is solved

at hand. So, for example, if I chose to run the ‘2d-tests/battery_term’ simulation for an

arbitrary number of time-steps and then choose to examine the diagnostics, am I correct

in assuming the following:

1) [Brms] = Gauss (as output by unit_magnetic, before the run begins)

2) [t] = s (since the default unit system is left as CGS)

3) [urms] = cm/s (again, as output by unit_velocity, before the run begins)

4) and etc. for the units of the other diagnostics

A: Detailed correspondence on this item can be found on:

https://groups.google.com/forum/?fromgroups#!topic/pencil-code-discuss/zek-uYNbgXI

There is also working material on unit systems under

http://www.nordita.org/~brandenb/teach/PencilCode/MixedTopics.html with a link to

http://www.nordita.org/~brandenb/teach/PencilCode/material/AlfvenWave_SIunits/

Below is a pedagogical response from Wlad Lyra:

In the sample battery-term, the sound speed cs0=1 sets the unit of

velocity. Together with the unit of length, that sets your unit of

time. The unit of magnetic field follows from the unit of velocity,

density, and your choice of magnetic permittivity, according to the

definition of the Alfven velocity.

If you are assuming cgs, you are saying that your sound speed cs0=1

actually means [U]=1 cm/s. Your unit of length is equivalently 1 cm,

and therefore the unit of time is [t] = [L]/[U]=1 s. The unit of

density is [rho] = 1 g/cm^3. Since in cgs vA=B/sqrt(4*pi * rho), your

unit of magnetic field is [B] = [U] * sqrt([rho] * 4*pi) ~= 3.5

sqrt(g/cm) / s = 3.5 Gauss.

If instead you are assuming SI, you have cs0=1 assuming that means

[U]=1 m/s and rho0=1 assuming that to mean [rho]=1 kg/m^3. Using [L]=1

m, you have still [t]=1 s, but now what appears as B=1 in your output

is actually [B] = [U] * sqrt (mu * [rho]) = 1 m/s * sqrt(4*pi * 1e-7

N*A-2 1 kg/m^3) ~= 0.0011210 kg/(s^2*A) ~ 11 Gauss.

You can make it more interesting and use units relevant to the

problem. Say you are at the photosphere of the Sun. You may want to

use dimensionless cs0=1 meaning a sound speed of 10 km/s. Your

appropriate length can be a megameter. Now your time unit is

[t]=[L]/[U] = 1e3 km/ 10 km/s = 10^2 s, i.e., roughly 1.5 minute. For

density, assume rho=2x10-4 kg/m^3, typical of the solar photosphere.

Your unit of magnetic field is therefore [B] = [U] * sqrt([rho] *

4*pi) = 1e6 cm/s * sqrt(4*pi * 2e-7 g/cm^3) ~ 1585.33 Gauss.

Notice that for mu0=1 and rho0=1 you simply have vA=B. Then you can

conveniently set the field strength by your choice of plasma beta (=

7.5 Visualization 87

2*cs^2/vA^2). There’s a reason why we like dimensionless quantities!

7.5 Visualization

7.5.1 ‘start.pro’ doesn’t work:

Reading grid.dat..

Reading param.nml..

\% Expression must be a structure in this context: PAR.

\% Execution halted at: \$MAIN\$ 104

/home/brandenb/pencil-code/runs/forced/hel1/../../../idl/start.pro

A: You don’t have the subdirectory ‘data’ in your IDL variable

!path

. Make sure you

source ‘sourceme.csh’/‘sourceme.sh’ or set a sufﬁcient IDL path otherwise.

7.5.2 ‘start.pro’ doesn’t work:

Isn’t there some clever (or even trivial) way that one can avoid the annoying error mes-

sages that one gets, when running e.g. ”.r rall” after a new variable has been introduced

in ”idl/varcontent.pro”? Ever so often there’s a new variable that can’t be found in my

param2.nml – this time it was IECR, IGG, and ILNTT that I had to circumvent. . .

A: The simplest solution is to invoke ‘NOERASE’, i.e. say

touch NOERASE

start.csh

or, alternatively, start_run.csh. What it does is that it reruns src/start.x with a new

version of the code; this then produces all the necessary auxiliary ﬁles, but it doesn’t

overwrite or erase the ‘var.dat’ and other ‘VAR’ and ‘slice’ ﬁles.

7.5.3 Something about tag name undeﬁned:

Q: In one of my older run directories I can’t read the data with idl anymore. What should

I do? Is says something like

Reading param.nml..

% Tag name LEQUIDIST is undefined for structure <Anonymous>.

% Execution halted at: $MAIN$ 182

/people/disk2/brandenb/pencil-code/idl/start.pro

A: Go into ‘data/param.nml’ and add , LEQUIDIST=T anywhere in the ﬁle (but before the

last slash).

7.5.4 Something INC in start.pro

Q: start doesn’t even work:

88 THE PENCIL CODE

% Compiled module: $MAIN$.

nname= 11

Reading grid.dat..

Reading param.nml..

Can’t locate Namelist.pm in INC (INC contains: /etc/perl /usr/local/lib/perl/5.8.4 /usr/local/share/perl/5.8.4

BEGIN failed--compilation aborted at /home/brandenb/pencil-code/bin/nl2idl line 49.

A: Go into ‘$PENCIL_HOME’ and say svn up sourceme.csh and/or svn up sourceme.sh.

(They were just out of date.)

7.5.5 nl2idl problem when reading param2.nml

Q: Does anybody encounter a backward problem with nl2idl? The ﬁle param*.nml ﬁles

are checked in under ‘pencil-code/axel/couette/SStrat128a_mu0.20_g2’ and the prob-

lem is below.

at /people/disk2/brandenb/pencil-code/bin/nl2idl line 120

HCOND0= 0.0,HCOND1= 1.000000,HCOND2= 1.000000,WIDTHSS= 1.192093E-06,MPOLY0=

^------ HERE

at /people/disk2/brandenb/pencil-code/bin/nl2idl line 120

A: The problem is the stupid ifc compiler writing the following into the namelist ﬁle:

COOLING_PROFILE=’gaussian ’,COOLTYPE=’Temp

’COOL= 0.0,CS2COOL= 0.0,RCOOL= 1.000000,WCOOL= 0.1000000,FBOT= 0.0,CHI_T= 0.0

If you add a comma after the closing quote:

COOLING_PROFILE=’gaussian ’,COOLTYPE=’Temp

’,COOL= 0.0,CS2COOL= 0.0,RCOOL= 1.000000,WCOOL= 0.1000000,FBOT= 0.0,CHI_T= 0.0

things will work.

Note that ifc cannot even itself read what it is writing here, so if this happened to occur

in param.nml, the code would require manual intervention after each start.csh.

7.5.6 Spurious dots in the time series ﬁle

Q: Wolfgang, you explained it to me once, but I forget. How can one remove spurious

dots after the timestep number if the time format overﬂows?

A: I don’t know whether it exists anywhere, but it’s easy. In Perl you’d say

perl -pe ’s/^(\s*[-0-9]+)\.([-0-9eEdD])/$1 $2/g’

and in sed (but that’s harder to read)

sed ’s/^$ *[-0-9]\+$\.$[-0-9eEdD]$/\1 \2/g’

7.5.7 Problems with pc_varcontent.pro

7.6 General questions 89

% Subscript range values of the form low:high must be >= 0, < size, with low

<= high: VARCONTENT.

% Error occurred at: PC_VARCONTENT 391

/home/brandenb/pencil-code/idl/read/pc_varcontent.pro

% PC_READ_VAR 318

/home/brandenb/pencil-code/idl/read/pc_read_var.pro

% $MAIN$

A: Make sure you don’t have any unused items in your src/cparam.local such as

! MAUX CONTRIBUTION 3

! COMMUNICATED AUXILIARIES 3

They would leave gaps in the counting of entries in your data/index.pro ﬁle.

7.6 General questions

7.6.1 “Installation” procedure

Why don’t you use GNU

autoconf/automake

for installation of the PENCIL CODE?

A: What do you mean by “installation”? Unlike the applications that normally use

auto-

conf

, the

Pencil Code

is neither a binary executable, nor a library that you compile once

and then dump somewhere in the system tree.

Autoconf

is the right tool for these appli-

cations, but not for numerical codes, where the typical compilation and usage pattern is

very different:

You have different directories with different ‘Makefile.local’ settings, recompile after

introducing that shiny new term in your equations, etc. Moreover, you want to some-

times switch to a different compiler (but just for that run directory) or another

MPI

implementation. Our adapt-mkfile approach gives you this ﬂexibility in a reasonably

convenient way, while doing the same thing with

autoconf

would be using that system

against most of its design principles.

Besides, it would really get on my (WD’s) nerves if I had to wait two minutes for

autoconf

to ﬁnish before I can start compiling (or maybe 5–10 minutes if I worked on a NEC

machine. . . ).

Finally, if you have ever tried to ﬁgure out what a ‘configure’ script does, you will ap-

preciate a comprehensible conﬁguration system.

7.6.2 Small numbers in the code

What is actually the difference between epsi, tini and tiny?

F90 has two functions epsilon() and tiny(), with

epsilon(x) = 1.1920929e-07

tiny(x) = 1.1754944e-38

(and then there is huge(x) = 3.4028235e+38)

90 THE PENCIL CODE

for a single-precision number x.

epsilon(x) is the smallest number that satisfies

1+epsilon(1.) /= 1 ,

while tiny(x) is the smallest number that can be represented without

precision loss.

In the code we have variants hereof,

epsi=5*epsilon(1.0)

tini=5*tiny(1.0)

huge1=0.2*huge(1.0)

that have added safety margins, so we don’t have to think about doing

things like 1/tini.

So in sub.f90,

- evr = evr / spread(r_mn+epsi,2,3)

did (minimally) affect the result for r_mn=O(1), while the correct version

+ evr = evr / spread(r_mn+tini,2,3)

only avoids overflow.

7.6.3 Why do we need a /lphysics/ namelist in the ﬁrst place?

Wolfgang answered on 29 July 2010: “‘cdata.f90’ has the explanation”

! Constant ’parameters’ cannot occur in namelists, so in order to get the

! now constant module logicals into the lphysics name list...

! We have some proxies that are used to initialize private local variables

! called lhydro etc, in the lphysics namelist!

So the situation is this: we want to write parameters like ldensity to param.nml so

IDL (and potentially octave, python, etc.) can know whether density was on or not. To

avoid confusion, we want them to have exactly their original names. But we cannot

assemble the original ldensity etc. constants in a namelist, so we have to deﬁne a local

ldensity variable. And to provide it with the value of the original cdata.ldensity, we need

to transfer the value via

ldensity var

. That’s pretty scary, although it seems to work

ﬁne. I can track the code back to the big

eos merger

commit, so it may originate from

that branch. One obvious problem is that you have to add code in a number of places

(the ldensity →

ldensity var

assignment and the local deﬁnition of ldensity) to really

get what you need. And when adding a new boolean of that sort to ‘cdata.f90’, you may

not even have a clue that you need all the other voodoo.

There may be a cleaner solution involving generated code. Maybe something like

logical :: ldensity ! INCLUDE_IN_LPHYSICS

could later generate code (in some param io extra.inc ﬁle) that looks like this:

write(unit, *) ’ldensity = ’, ldensity

i.e. we can manually write in namelist format. But maybe there are even simpler solu-

tions?

7.6 General questions 91

7.6.4 Can I run the code on a Mac?

A: Macs work well for Linux stuff, except that the ﬁle structure is slightly different.

Problems when following Linux installs can usually be traced to the PATH. For general

reference, if you need to set an environment variable for an entire OS-X login session,

google environment.plist. That won’t be needed here.

For a Mac install, the following should work:

a) Install Dev Tools (an optional install on the MacOS install disks). Unfortunately,

last time I checked the svn version that comes with DevTools is obsolete. So:

b) Install MacPorts (download from web). Note that MacPorts installs to a non-

standard location, and will need to be sourced. The installation normally drops

an appropriate line in .proﬁle. If it does so, make sure that that line gets sourced.

Otherwise

export PATH=/opt/local/bin:/opt/local/sbin:$PATH

export MANPATH=/opt/local/share/man:$MANPATH

c) Install g95 (download from web). Make sure it is linked in /bin.

d) execute macports svn install

e) download the pencil-code and enjoy.

Note: the above way to get svn works. It takes a while however, so there are certainly

faster ways out there. If you already have a non-obsolete svn version, use that instead.

7.6.5 Pencil Code discussion forum

Do I just need to send an email somewhere to subscribe or what?

A” The answer is yes; just go to:

http://groups.google.com/group/pencil-code-discuss

7.6.6 The manual

It would be a good idea to add this useful information in the manual, no?

A: When you have added new stuff to the code, don’t forget to mention this in the

‘pencil-code/doc/manual.tex’ ﬁle.

Again, the answer is yes; just go to:

cd pencil-code/doc/

vi manual.tex

svn ci -m "explanations about a new module in the code"

92 THE PENCIL CODE

Part II

Programming the PENCIL CODE

All developers are supposed to have an up-to-date entry in the ﬁle

‘pencil-code/license/developers.txt’ so that they can be contacted in case a code

change breaks an auto-test or other code functionality.

Several PENCIL CODE committers have done several hundred check-ins, but many of

the currently 68 registered people on the repository have hardly done anything. To put

a number to this, one can deﬁne an hindex, which gives the number of users, who have

done at least as many as that number of check-ins. This hindex is currently 32, i.e., 32

users have done at least 32 check-ins; see Figure 6.

Figure 6: The hindex of PENCIL CODE check-ins.

The PENCIL CODE has expanded approximately linearly in the number of lines of code

and the number of subroutines (Fig. 7). The increase in the functionality of the code is

documented by the rise in the number of sample problems (Fig. 8). It is important to

monitor the performance of the code as well. Figure 9 shows that for most of the runs

the run time has not changed much.

Before making changes to the code, it is important that you verify that you can run

the pc_auto-test successfully. Don’t do this when you have already modiﬁed the code,

because then you cannot be sure that any problems are caused by your changes, or

because it wouldn’t have worked anyway. Also, keep in mind that the code is public,

so your changes should make sense from a broader perspective and should not only

be intended for yourself. Regarding more general aspects about coding standards see

Sect. B.2.

In order to keep the development of the code going, it is important that the users are

able to understand and modify (program!) the code. In this section we explain ﬁrst how

94 THE PENCIL CODE

Figure 7: Number of lines of code and the number of subroutines since the end of 2001. The jump in the

Summer of 2005 was the moment when the developments on the side branch (eos branch) were merged

with the main trunk of the code. Note the approximately linear scaling with time.

to orient yourself in the code and to understand what is in it, and then to modify it

according to your needs.

The Pencil Code check-ins occur regularly all the time. By the Pencil Code User Meeting

2010 we have arrived at a revision number of 15,000. In February 2017, the number of

check-ins has risen to 26,804; see https://github.com/pencil-code/pencil-code. Ma-

jor code changes are nowadays being discussed by the Pencil Code Steering Committee

(https://www.nordita.org/~brandenb/pencil-code/PCSC/). The increase of the revision

number with time is depicted in Figure 10. The number of Pencil Code developers in-

creases too (Figure 11), but the really active ones are getting rare. This may indicate

that new users can produce new science with the code as it is, but it may also indicate

that it is getting harder to understand the code. How to understand the code will be

discussed in the next section.

Figure 8: Number of tests in the sample directory that are used in the nightly auto tests. Note again the

approximately linear scaling with time.

Figure 9: Run time of the daily auto-tests since August 17, 2008. For most of the runs the run time has

not changed much. The occasional spikes are the results of additional load on the machine.

96 THE PENCIL CODE

Figure 10: Number of check-ins since 2002. Note again the linear increase with time, although in the last

part of the time series there is a notable speed-up.

Figure 11: Check-ins since 2002 per user. Users with more than 100 check-ins are color coded.

8. Understanding the code 97

8 Understanding the code

Understanding the code means looking through the code. This is not normally done by

just printing out the entire code, but by searching your way through the code in order to

address your questions. The general concept will be illustrated here with an example.

8.1 Example: how is the continuity equation being solved?

All the physics modules are solved in the routine pde, which is located in the ﬁle and

module ‘Equ’. Somewhere in the pde subroutine you ﬁnd the line

call dlnrho_dt(f,df,p)

This means that here the part belonging to ∂ln ρ/∂t is being assembled. Using the grep

command you will ﬁnd that this routine is located in the module density, so look in

there and try to understand the pieces in this routine. We quickly arrive at the following

crucial part of code,

! Continuity equation.

if (lcontinuity_gas) then

if (ldensity_nolog) then

df(l1:l2,m,n,irho) = df(l1:l2,m,n,irho) - p%ugrho - p%rho*p%divu

else

df(l1:l2,m,n,ilnrho) = df(l1:l2,m,n,ilnrho) - p%uglnrho - p%divu

endif

where, depending on some logicals that tell you whether the continuity equation should

indeed be solved and whether we do want to solve for the logarithmic density and not

the actual density, the correct right hand side is being assembled. Note that all these

routines always only add to the existing df(l1:l2,m,n,ilnrho) array and never reset

it. Resetting df is only done by the timestepping routine. Next, the pieces p%uglnrho

and p%divu are being subtracted. These are pencils that are organized in the structure

with the name p. The meaning of their names is obvious: uglnrho refers to u· ∇ln ρ

and divu refers to ∇ · u. In the subroutine pencil_criteria_density you ﬁnd under

which conditions these pencils are requested. Using grep, you also ﬁnd where they are

calculated. For example p%uglnrho is calculated in ‘density.f90’; see

call u_dot_grad(f,ilnrho,p%glnrho,p%uu,p%uglnrho,UPWIND=lupw_lnrho)

So this is a call to a subroutine that calculates the u·∇ operator, where there is the possi-

bility of

upwinding

, but this is not the default. The piece divu is calculated in ‘hydro.f90’

in the line

! Calculate uij and divu, if requested.

if (lpencil(i_uij)) call gij(f,iuu,p%uij,1)

if (lpencil(i_divu)) call div_mn(p%uij,p%divu,p%uu)

98 THE PENCIL CODE

Note that the divergence calculation uses the velocity gradient matrix as input, so no

new derivatives are recalculated. Again, using grep, you will ﬁnd that this calculation

and many other ones happen in the module and ﬁle ‘sub.f90’. The various derivatives

that enter here have been calculated using the gij routine, which calls the der routine,

e.g., like so

k1=k-1

do i=1,3

do j=1,3

if (nder==1) then

call der(f,k1+i,tmp,j)

For all further details you just have to follow the trail. So if you want to know how the

derivatives are calculated, you have to look in deriv.f90, and only here is it where the

indices of the farray are being addressed.

If you are interested in magnetic ﬁelds, you have to look in the ﬁle ‘magnetic.f90’. The

right hand side of the equation is assembled in the routine

!***********************************************************************

subroutine daa_dt(f,df,p)

! Magnetic field evolution.

! Calculate dA/dt=uxB+3/2 Omega_0 A_y x_dir -eta mu_0 J.

! For mean field calculations one can also add dA/dt=...+alpha*bb+delta*WXJ.

! Add jxb/rho to momentum equation.

! Add eta mu_0 j2/rho to entropy equation.

where the header tells you already a little bit of what comes below. It is also here where

ohmic heating effects and other possible effects on other equations are included, e.g.

! Add Ohmic heat to entropy or temperature equation.

if (lentropy .and. lohmic_heat) then

df(l1:l2,m,n,iss) = df(l1:l2,m,n,iss) &

+ etatotal*mu0*p%j2*p%rho1*p%TT1

endif

We leave it at this and encourage the user to do similar inspection work on

a number of other examples. If you think you ﬁnd an error, ﬁle a ticket at

http://code.google.com/p/pencil-code/issues/list. You can of course also repair it!

9. Adapting the code 99

9 Adapting the code

9.1 The PENCIL CODE coding standard

As with any code longer than a few lines the appearance and layout of the source code

is of the utmost importance. Well laid out code is more easy to read and understand and

as such is less prone to errors.

A consistent coding style has evolved in the PENCIL CODE and we ask that those con-

tributing try to be consistent for everybody’s beneﬁt. In particular, it would be appreci-

ated if those committing changes of existing code via svn follow the given coding style.

There are not terribly many rules and using existing code as a template is usually the

easiest way to proceed. In short the most important rules are:

•tab characters do not occur anywhere in the code (in fact the use of tab character

is an extension to the Fortran standard).

•Code in any delimited block, e.g. if statements, do loops, subroutines etc., is in-

dented be precisely 2 spaces. E.g.

if (lcylindrical) then

call fatal_error(’del2fjv’,’del2fjv not implemented’)

endif

•continuation lines (i.e. the continuation part of a logical line that is split using

the & sign) are indented by 4 spaces. E.g. (note the difference from the previous

example)

if (lcylindrical) &

call fatal_error(’del2fjv’,’del2fjv not implemented’)

[...]

•There is always one space separation between ’if ’ and the criterion following in

parenthesis:

if (ldensity_nolog) then

rho=f(l1:l2,m,n,irho)

endif

This is wrong:

if(ldensity_nolog) then ! WRONG

rho=f(l1:l2,m,n,irho)

endif

•In general, try to follow common practice used elsewhere in the code. For example,

in the code fragment above there are no empty spaces within the mathematical

expressions programmed in the code. A unique convention helps in ﬁnding certain

expressions and patterns in the code. However, empty spaces are often used after

commas and semicolons, for examples in name lists.

•Relational operators are written with symbols (==,/=,<,<=,>,>=), not with

characters (.eq.,.ne.,.lt.,.le.,.gt.,.ge.).

•In general all comments are placed on their own lines with the ’!’ appearing in the

ﬁrst column.

100 THE PENCIL CODE

•All subroutine/functions begin with a standard comment block describing what

they do, when and by whom they were created and when and by whom any non-

trivial modiﬁcations were made.

•Lines longer that 78 characters should be explicitly wrapped using the & character,

unless there is a block of longer lines that can only be read easily when they are

not wrapped. Always add one whitespace before the & character.

These and other issues are discussed in more depth and with examples in Appendix B,

and in particular in Sect. B.2.

9.2 Adding new output diagnostics

With the implementation of new physics and the development of new procedures it will

become necessary to monitor new diagnostic quantities that have not yet been imple-

mented in the code. In the following, we describe the steps necessary to set up a new

diagnostic variable.

This is nontrivial as, in order to keep latency effects low on multi-processor machines,

the code minimizes the number of global reduction operations by assembling all quan-

tities that need the maximum taken in

fmax

, and those that need to be summed up

over all processors (mostly for calculating mean quantities) in

fsum

(see subroutine

diagnostic in ﬁle ‘src/equ.f90’).

As a sample variable, let us consider

jbm

(the volume average j·B). Only the mod-

ule

magnetic

will be affected, as you can see (the diagnostic quantity

jbm

is already

implemented) with

unix> grep -i jbm src/*.f90

If we pretend for the sake of the exercise that no trace of

jbm

was in the code, and we

were only now adding it, we would need to do the following

1. add the variable

idiag jbm

to the module variables of

Magnetic

in both

‘magnetic.f90’ and ‘nomagnetic.f90’:

integer :: idiag_jbm=0

The variable

idiag jbm

is needed for matching the position of

jbm

with the list of

diagnostic variables speciﬁed in ‘print.in’.

2. in the subroutine daa_dt in ‘magnetic.f90’, declare and calculate the quantity

(the average of which will be

jbm

), and call sum_mn_name

real, dimension (nx) :: jb

! jj

[. . . ]

if (ldiagnos) then

! only calculate if diagnostics is required

if (idiag_jbm/=0) then

! anybody asked for jbm?

call dot_mn(jj,bb,jb)

! assuming jj and bb are known

call sum_mn_name(jb,i_jbm)

endif

9.2 Adding new output diagnostics 101

3. in the subroutine rprint_magnetic in both ‘magnetic.f90’, add the following:

! reset everything in case of RELOAD

! (this needs to be consistent with what is defined above!)

if (lreset) then

! need to reset list of diagnostic variables?

[. . . ]

idiag_jbm=0

[. . . ]

endif

! check for those quantities that we want to evaluate online

do iname=1,nname

[. . . ]

call parse_name(iname,cname(iname),cform(iname),’jbm’,idiag_jbm)

[. . . ]

enddo

[. . . ]

! write column, i_XYZ, where our variable XYZ is stored

[. . . ]

write(3,*) ’i_jbm=’,idiag_jbm

[. . . ]

4. in the subroutine rprint_magnetic in ‘nomagnetic.f90’, add the following (newer

versions of the code may not require this any more):

! write column, i_jbm, where our variable jbm is stored

! idl needs this even if everything is zero

[. . . ]

write(3,*) ’i_jbm=’,idiag_jbm

[. . . ]

5. and don’t forget to add your new variable to ‘print.in’:

jbm(f10.5)

If, instead of a mean value, you want a new maximum quantity, you need to replace

sum_mn_name() by max_mn_name().

Sect. 5.8.1 describes how to output horizontal averages of the magnetic and velocity

ﬁelds. New such averages can be added to the code by using the existing averaging

procedures calc_bmz() or calc_jmz() as examples.

102 THE PENCIL CODE

9.3 The f-array

The ‘f’ array is the largest array in the PENCIL CODE and its primary role is to store

the current state of the timestepped PDE variables. The f-array and its slightly smaller

counter part (the df-array; see below) are the only full size 3D arrays in the code. The

f-array is of type real but PDEs for a complex variable may be solved by using two

slots in the f-array. The actual size of the f-array is mx ×my ×mz ×mfarray. Here,

mfarray = mvar + maux + mglobal + mscratch where mvar refers to the number of real PDE

variables.

As an example, we describe here how to put the time-integrated velocity,

uut

, into the

f-array (see ‘hydro.f90’). If this is to be invoked, there must be the following call some-

where in the code:

call farray_register_auxiliary(’uut’,iuut,vector=3)

Here,

iuut

is the index of the variable

uut

in the f-array. Of course, this requires that

maux

is increased by 3, but in order to do this for a particular run only one must write

a corresponding entry in the ‘cparam.local’ ﬁle,

! -*-f90-*- (for Emacs)

! cparam.local

!** AUTOMATIC CPARAM.INC GENERATION ****************************************

! Declare (for generation of cparam.inc) the number of f array

! variables and auxiliary variables added by this module

! MAUX CONTRIBUTION 3

!***************************************************************************

! Local settings concerning grid size and number of CPUs.

! This file is included by cparam.f90

integer, parameter :: ncpus=1,nprocy=1,nprocz=ncpus/nprocy,nprocx=1

integer, parameter :: nxgrid=16,nygrid=nxgrid,nzgrid=nxgrid

This way such a change does not affect the memory usage for other applications where

this addition to ‘cparam.local’ is not made. In order to output this part of the f-array,

one must write

lwrite aux=T

in the init_pars of ‘start.in’. (Technically, [lwrite -

aux]lwrite aux=T can also be invoked in run_pars of ‘run.in’, but this does not work

at the moment.)

9.4 The df-array

The ‘df’ array is the second largest chunk of data in the PENCIL CODE. By using a 2N

storage scheme (see H.4) after Williamson [33] the code only needs one more storage

area for each timestepped variable on top of the current state stored in the f-array. As

such, and in contrast to the f-array, the df-array is of size mx ×my ×mz ×mvar. Like the

df-array it is of type real. In fact the ghost zones of df are not required or calculated but

having f- and df-arrays of the same size make the coding more transparent. For mx,my

and mz large the wasted storage becomes negligible.

9.5 The fp-array 103

9.5 The fp-array

Similar to the ‘f’ array the code also has a ’fp’ array which contains current states of

all the particles. Like the f-array the fp-array also has a time derivative part, the dfp-

array. The dimension of the fp-array is mparlocal ×mpvar where mparlocal is the number

of particles in the local processor (for serial runs this is the total number of particles)

and mpvar depends on the problem at hand. For example if we are solving for only

tracer particles then mpvar = 3, for dust particles mpvar = 6 The sequence in which the

slots in the fp-array are ﬁlled up depends on the sequence in which different particle

modules are called from the particles_main.f90. The following are the relevant lines

from particles_main.f90.

!***********************************************************************

subroutine particles_register_modules()

! Register particle modules.

! 07-jan-05/anders: coded

call register_particles ()

call register_particles_radius ()

call register_particles_spin ()

call register_particles_number ()

call register_particles_mass ()

call register_particles_selfgrav ()

call register_particles_nbody ()

call register_particles_viscosity ()

call register_pars_diagnos_state ()

endsubroutine particles_register_modules

!***********************************************************************

The subroutine resister_particles can mean either the tracer particles or dust parti-

cles. For the former the ﬁrst three slots of the fp-array are the three spatial coordinates.

For the latter the ﬁrst six slots of the fp-array are the three spatial coordinates followed

by the three velocity components. The seventh slot (or the fourth if we are use tracer

particles) is the radius of the particle which can also change as a function of time as

particles collide and fuse together to form bigger particles.

9.6 The pencil case

Variables that are derived from the basic physical variables of the code are stored in

one-dimensional

pencils

of length

. All the pencils that are deﬁned for a given set

of physics modules are in turn bundled up in a Fortran structure called p(or, more

illustrative, the

pencil case

). Access to individual pencils happens through the variable

p%name, where name is the name of a pencil, e.g. rho that is a derived variable of the

logarithmic density lnrho.

The pencils provided by a given physics module are declared in the header of the ﬁle,

e.g. in the Density module:

104 THE PENCIL CODE

! PENCILS PROVIDED lnrho; rho; rho1; glnrho(3); grho(3); uglnrho; ugrho

Notice that the pencil names are separated with a semi-colon and that vector pencils

are declared with “(3)” after the name. Before compiling the code, the script ‘mkcparam’

collects the names of all pencils that are provided by the chosen physics modules. It

then deﬁnes the structure pwith slots for every single of these pencils. The deﬁni-

tion of the pencil case pis written in the include ﬁle ‘cparam_pencils.inc’. When the

code is run, the actual pencils that are needed for the run are chosen based on the in-

put parameters. This is done in the subroutines pencil_criteria_modulename that are

present in each physics module. They are all called once before entering the time loop.

In the pencil_criteria subroutines the logical arrays lpenc_requested,lpenc_diagnos,

lpenc_diagnos2d, and lpenc_video are set according to the pencils that are needed for

the given run. Some pencils depend on each other, e.g. uglnrho depends on uu and glnrho.

Such interdependencies are sorted out in the subroutines pencil_interdep_modulename

that are called after pencil_criteria_modulename.

In each time-step the values of the pencil logicals lpenc_requested,lpenc_diagnos,

lpenc_diagnos2d, and lpenc_video are combined to one single pencil array lpencil

which is different from time-step to time-step depending on e.g. whether diagnostics

or video output are done in that time-step. The pencils are then calculated in the sub-

routines calc_pencils_modulename. This is done before calculating the time evolution of

the physical variables, as this depends very often on derived variables in pencils.

The centralized pencil calculation scheme is a guarantee that

•All pencils are only calculated once

•Pencils are always calculated by the proper physics module

Since the PENCIL CODE is a multipurpose code that has many different physics mod-

ules, it can lead to big problems if a module tries to calculate a derived variable that

actually belongs to another module, because different input parameters can inﬂuence

how the derived variables are calculated. One example is that the Density module can

consider both logarithmic and non-logarithmic density, so if the Magnetic module calcu-

lates

rho = exp(f(l1:l2,m,n,ilnrho)

it is wrong if the Density module works with non-logarithmic density! The proper way

for the Magnetic module to get to know the density is to request the pencil rho in

pencil_criteria_magnetic.

9.6.1 Pencil check

To check that the correct pencils have been requested for a given run, one can run a

pencil consistency check

in the beginning of a run by setting the logical lpencil_check

in &run_pars. The check is meant to see if

•All needed pencils have been requested

•All requested pencils are needed

The consistency check ﬁrst calculates the value of df with all the requested pencils. Then

the pencil requests are ﬂipped one at a time – requested to not requested, not requested

to requested. The following combination of events can occur:

9.7 Adding new physics: the Special module 105

•not requested →requested, df not changed

The pencil is not requested and is not needed.

•not requested →requested, df changed

The pencil is not requested, but is needed. The code stops.

•requested →not requested, df not changed

The pencil is requested, but is not needed. The code gives a warning.

•requested →not requested, df changed

The pencil is requested and is needed.

9.6.2 Adding new pencils

Adding a new pencil to the pencil case is trivial but requires a few steps.

•Declare the name of the pencil in the header of the proper physics module. Pencils

names must appear come in a ”;” separated list, with dimensions in parenthesis

after the name [(3) for vector, (3,3) for matrix, etc.].

•Set interdependency of the new pencil (i.e. what other pencils does it depend on) in

the subroutine pencil_interdep_modulename

•Make rule for calculating the pencil in calc_pencils_modulename

•Request the new pencil based on the input parameters in any relevant physics

module

Remember that the centralized pencilation scheme is partially there to force the users

of the code to think in general terms when implementing new physics. Any derived

variable can be useful for a number of different physics problems, and it is important

that a pencil is accessible in a transparent way to all modules.

9.7 Adding new physics: the Special module

If you want to add new physics to the code, you will in many cases want to add a new

Special module. Doing so is relatively straight forward and there is even a special direc-

tory for such additions.

To create your own special module, copy ‘nospecial.f90’ from the src/ directory to a

new name in the src/special/ directory. It is currently only possible to have one special

modules at a time and so several new bits of physics are often put in to one special

module. For this reasons a name should be chosen that relates to the problem to be

solved rather than the speciﬁc physics being implemented.

The ﬁrst thing to do in your new module is to change the lspecial=.false. header to say

lspecial=.true.

The ﬁle is heavily commented though all such comments can be removed as you go. You

may implement any of the subroutines/function that exist in

nospecial.f90

and those

routines must have the names and parameters as in

nospecial.f90

. You do not how-

ever need to implement all routines, and you may either leave the dummy routines

106 THE PENCIL CODE

copied from

nospecial.f90

or delete them all together (provided the ”include ’special -

dummy.inc’” is kept intact at the end of the ﬁle. Beyond that, and data and subroutines

can be added to a special module as required, though only for use within that module.

There are routines in the special interface to allow you to add new equations, modify the

existing equation, add diagnostics, add slices, and many more things. If you feel there is

something missing extra hooks can easily be added - please contact the PENCIL CODE

team for assistance.

You are encouraged to submit/commit your special modules to the Pencil Code source.

When you have added new stuff to the code, don’t forget to mention this in the

‘pencil-code/doc/manual.tex’ ﬁle.

9.8 Adding switchable modules

In some cases where a piece of physics is thought to be more fundamental, useful in

many situations or simply more ﬂexibility is required it may be necessary to add a new

module

newphysics

together with the corresponding

nonewphysics

module. The special

modules follow the same structure as the rest of the switchable modules and so using a

special module to prototype new ideas can make writing a new switchable module much

easier.

For an example of module involving a new variable (and PDE), the

pscalar

module is a

good prototype. The grep command

unix> grep -i pscalar src/*

gives you a good overview of which ﬁles you need to edit or add.

9.9 Adding your initial conditions: the InitialCondition module

Although the code has many initial conditions implemented, we now discourage such

practice. We aim to eventually removed most of them. The recommended course of action

is to make use of the InitialCondition module.

InitialCondition works pretty much like the Special module. To implement your own

custom initial conditions, copy the ﬁle ‘noinitial_condition.f90’ from the src/ to src/

initial_condition, with a new, descriptive, name.

The ﬁrst thing to do in your new module is to change the linitialcondition=.false. header

to say linitialcondition=.true. Also, don’t forget to add ../ in front of the ﬁle names in

include statements.

This ﬁle has hooks to implement a custom initial condition to most vari-

ables. After implementing your initial condition, add the line INITIAL_-

CONDITION=initial_condition/myinitialcondition to your ‘src/Makefile.local’

ﬁle. Here, myinitialcondition is the name you gave to your initial condition ﬁle. Add

also initial_condition_pars to the ‘start.in’ ﬁle, just below init_pars. This is a

namelist, which you can use to add whichever quantity your initial condition needs

deﬁned, or passed. You must also un-comment the relevant lines in the subroutines

for reading and writing the namelists. For compiling reasons, these subroutines in

‘noinitial_condition.f90’ are dummies. The lines are easily identiﬁable in the code.

9.9 Adding your initial conditions: the InitialCondition module 107

Check e.g. the samples ‘2d-tests/baroclinic’, ‘2d-tests/spherical_viscous_ring’, or

‘interlocked-fluxrings’, for examples of how the module is used.

108 THE PENCIL CODE

10 Testing the code

To maintain reproducibility despite sometimes quite rapid development, the PENCIL

CODE is tested nightly on various architectures. The front end for testing are the scripts

pc_auto-test and (possibly) pencil-test.

To see which samples would be tested, run

unix> pc_auto-test -l

, to actually run the tests, use

unix> pc_auto-test

unix> pc_auto-test --clean

. The latter compiles every test sample from scratch and currently (September 2009)

takes about 2 hours on a mid-end Linux PC.

The pencil-test script is useful for cron jobs and allows the actual test to run on a

remote computer. See Sect. 10.1 below.

For a complete list of options, run pc_auto-test --help and/or pencil-test --help.

10.1 How to set up periodic tests (auto-tests)

To set up a nightly test of the PENCIL CODE, carry out the following steps.

1. Identify a host for running the actual tests (the work host) and one to initiate

the tests and collect the results (the scheduling host). On the scheduling host, you

should be able to

(a) run cron jobs,

(b) ssh to the work host without password,

(d) send e-mail (optional, but recommended).

Work host and scheduling host can be the same (in this case, use pencil-test’s ‘-l’

option, see below), but often they will be two different computers.

2. [Recommended, but optional:] On the work host, check out a separate copy of the

PENCIL CODE to reduce the risk that you start coding in the auto-test tree. In the

following, we will assume that you checked out the code as ‘~/pencil-auto-test’.

3. On the work host, make sure that the code ﬁnds the correct conﬁguration ﬁle for

the tests you want to carry out. [Elaborate on that: PENCIL_HOME/local_config and

‘-f’ option; give explicit example]

Remember that you can set up a custom host ID ﬁle for your auto-test tree under

‘${PENCIL_HOME}/config-local/hosts/’.

4. On the scheduling host, use crontab -e to set up a

cron

job similar to the following:

10.1 How to set up periodic tests (auto-tests) 109

30 02 * * * $HOME/pencil-auto-test/bin/pencil-test \

-D $HOME/pencil-auto-test \

--use-pc_auto-test \

-N15 -Uc -rs \

-T $HOME/public_html/pencil-code/tests/timings.txt \

-t 15m

-m <email1@inter.net,email2@inter.net,...> \

<work-host.inter.net> \

-H > $HOME/public_html/pencil-code/tests/nightly-tests.html

Note 1: This has to be one long line. The backslash characters are written only

for formatting purposes for this manual you cannot use them in a crontab ﬁle.

Note 2: You will have to adapt some parameters listed here and may want to

modify a few more:

‘-D <dir>’: Sets the directory (on the work host) to run in.

‘-T <file>’: If this option is given, append a timing statistics line for each test to

the given ﬁle.

‘--use-pc’: You want this option (and at some point, it will be the default).

‘-t 15m’: Limit the time for ‘start.x’ and ‘run.x’ to 15 minutes.

‘-N 15’: Run the tests at nice level 15 (may not have an effect for MPI tests).

‘-Uc’: Do svn update and pc_build --cleanall before compiling.

‘-m <email-list>’: If this option is given, send e-mails to everybody in the

(comma-separated) list of e-mail addresses if any test fails. As soon as this

option is set, the maintainers (as speciﬁed in the ‘README’ ﬁle) of failed tests

will also receive an e-mail.

work-host.inter.net|-l:Replace this with the remote host that is to run the

tests. If you want to run locally, write -l instead.

‘-H’: Output HTML.

> $HOME/public_html/pencil-code/tests/nightly-tests.html:Write output to

the given ﬁle.

If you want to run fewer or more tests, you can use the ‘-Wa,--max-level’ option:

-Wa,--max-level=3

will run all tests up to (and including) level 3. The default corresponds to

‘-Wa,--max-level=2’.

For a complete listing of pencil-test options, run

unix> pencil-test --help

110 THE PENCIL CODE

11 Useful internals

11.1 Global variables

The following variables are deﬁned in ‘cdata.f90’ and are available in any routine that

uses the module

Cdata

Variable Meaning

real

simulated time t.

integer

n[xyz]grid

global number of grid points (excluding ghost cells)

in x,yand zdirection.

number of grid points (excluding ghost cells) as seen

by the current processor, i. e. ny=nygrid/nprocy, etc.

number of grid points seen by the current processor,

but including ghost cells. Thus, the total box for the

ivar

th variable (on the given processor) is given by

f(1:mx,1:my,1:mz,ivar).

smallest and largest x-index for the physical domain

(i. e. excluding ghost cells) on the given processor.

smallest and largest y-index for physical domain.

smallest and largest z-index for physical domain,

i. e. the physical part of the

ivar

th variable is given

by f(l1:l2,m1:m2,n1:n2,ivar)

pencil indexing variables: During each time-substep

the box is traversed in x-pencils of length

such

that the current pencil of the

ivar

th variable is

f(l1:l2,m,n,ivar).

logical

lroot

true only for MPI root processor.

lﬁrst

true only during ﬁrst time-substep of each time step.

headt

true only for very ﬁrst full time step (comprising 3

substeps for the 3rd-order Runge–Kutta scheme) on

root processor.

headtt

= (lfirst .and. lroot): true only during very ﬁrst

time-substep on root processor.

lﬁrstpoint

true only when the very ﬁrst pencil for a given time-

substep is processed, i. e. for the ﬁrst set of (

which is probably (3,3) .

lout

true when diagnostic output is about to be written.

11.2 Subroutines and functions

output(file,a,nv) (module

): Write (in each ‘procN’ directory) the content of the

global array ato a ﬁle called ﬁle, where ahas dimensions

, or

11.2 Subroutines and functions 111

if nv=1.

output_pencil(file,a,nv) (module

): Same as output(), but for a pencil variable,

i. e. an auxiliary variable that only ever exists on a pencil (e. g. the magnetic ﬁeld

strength

in ‘magnetic.f90’, or the squared sound speed

cs2

in ‘entropy.f90’).

The ﬁle has the same structure as those written by output(), because the values

of aon the different pencils are accumulated in the ﬁle. This involves a quite non-

trivial access pattern to the ﬁle and has thus been coded in

(‘src/debug_c.c’).

cross(a,b,c) (module

Sub

): Calculate the cross product of two vectors aand band

store in c. The vectors must either all be of size

×3 (global arrays), or

of size

×3 (pencil arrays).

dot(a,b,c) (module

Sub

): Calculate the dot product of two vectors aand band store

in c. The vectors must either be of size

×3 (aand b) and

(c), or of size

×3 (aand b) and

(c).

dot2(a,c) (module

Sub

): Same as dot(a,a,c).

112 THE PENCIL CODE

113

Part III

Appendix

APPENDIX Date, Revision

A Timings

In the following table we list the results of timings of the code on different machines.

Shown is (among other quantities) the wall clock time per mesh point (excluding the

ghost zones) and per full 3-stage time step, a quantity that is printed by the code at the

end of a run.16

As these results were assembled during the development phase of the code (that hasn’t

really ﬁnished yet,. . . ), you may not get the same numbers, but they should give some

orientation of what to expect for your speciﬁc application on your speciﬁc hardware.

The code will output the timing (in microseconds per grid point per time-step) at the

end of a run. You can also specify walltime in print.in to have the code continuously

output the physical time it took to reach the time-steps where diagnostics is done. The

time-dependent code speed can then be calculated by differentiating, e.g. in IDL with

IDL> pc_read_ts, obj=ts

IDL> plot, ts.it, 1/nw*deriv(ts.it,ts.walltime/1.0e-6), psym=2

where nw=nx*ny*nz.

proc machine µs

pt step resol. what mem/proc when who

1 Nl3 19 643kinematic 10 MB 20-may-02 AB

1 Nl3 30 643magn/noentro 20 MB 20-may-02 AB

1 Nq1 10 643magn/noentro 30-may-02 AB

1 Ukaff 9.2 643magn/noentro 20-may-02 AB

1 Nl6 6.8 643magn/noentro 10-mar-03 AB

1 Nl6 36.3 64×128×64 nomag/entro/dust 19-sep-03 AB

1 Nl6 42.7 162

×256 nomag/entro/rad6/ion 22-oct-03 AB

1 Nl6 37.6 162

×256 nomag/entro/rad2/ion 22-oct-03 AB

1 Nl6 19.6 162

×256 nomag/entro/ion 22-oct-03 AB

1 Nl6 8.7 162

×256 nomag/entro 22-oct-03 AB

1 Nl6n 9.8 323magn/noentro/pscalar 17-mar-06 AB

1 Mhd 7.8 643magn/noentro 20-may-02 AB

1 Nq4 14.4 1283magn/noentro 8-oct-02 AB

1 Nq5 6.7 1283magn/noentro 8-oct-02 AB

1 fe1 5.1 1283magn/noentro 9-oct-02 AB

1 Kabul 4.4 1283magn/noentro 130 MB 20-jun-02 WD

1 Hwwsx5 3.4 2563convstar 7.8 GB 29-jan-03 WD

1 Mac/g95 7.7 323magn/noentro 14-jan-07 BD

1 Mac/ifc 4.5 323magn/noentro 14-jan-07 BD

2 Kabul 2.5 1283magn/noentro 80 MB 20-jun-02 WD

2 Nq3+4 7.4 1283magn/noentro 8-oct-02 AB

2 Nq4+4 8.9 1283magn/noentro 8-oct-02 AB

2 Nq4+5 7.3 1283magn/noentro 8-oct-02 AB

2 Nq5+5 3.7 1283magn/noentro 8-oct-02 AB

16 Note that when using ‘nompicomm.f90’, the timer currently used will overﬂow on some machines, so

you should not blindly trust the timings given by the code.

114 THE PENCIL CODE

2 fe1 3.45 1283magn/noentro 9-oct-02 AB

2 Nq2 9.3 643magn/noentro 11-sep-02 AB

2 Nq1+2 8.3 643magn/noentro 11-sep-02 AB

2 Hwwsx5 1.8 2563convstar 7.9 GB 29-jan-03 WD

4 Nq1+2 5.4 643magn/noentro 11-sep-02 AB

4 Nq1235 4.1 1283magn/noentro 11-sep-02 AB

4 Nq0-3 6.8 2563magn/noentro 294 MB 10-jun-02 AB

4 Mhd 2.76 643magn/noentro 30-may-02 AB

4 fe1 3.39 323magn/noentro 16-aug-02 AB

4 Rasm. 2.02 643magn/noentro 2x2 8-sep-02 AB

4 Mhd 8.2 642

×16 nomag/entro 23-jul-02 AB

4 fe1 6.35 64×128×64 nomag/entro/dust 19-sep-03 AB

4 fe1 2.09 1283magn/noentro 9-oct-02 AB

4 fe1 1.45 1283magn/noentro giga 9-oct-02 AB

4 fe1 7.55 162

×512 nomag/entro/rad2/ion 4x1 1-nov-03 AB

4 fe1 5.48 162

×512 nomag/entro/rad2/ion 1x4 1-nov-03 AB

4 Luci 1.77 643magn/noentro 27-feb-07 AB

4 Lenn 0.65 643nomag/noentro 13-jan-07 AB

4 Lenn 1.21 643magn/noentro 7-nov-06 AB

4 Kabul 1.5 1283magn/noentro 47 MB 20-jun-02 WD

4 Hwwsx5 1.8 2563convstar 8.2 GB 29-jan-03 WD

8 Nqall 3.0 1283magn/noentro 8-oct-02 AB

8 fe1 3.15 643magn/noentro 1x8 8-sep-02 AB

8 fe1 2.36 643magn/noentro 2x4 8-sep-02 AB

8 Ukaff 1.24 643magn/noentro 20-may-02 AB

8 Kabul 1.25 642

×128 nomag/entro 11-jul-02 WD

8 fe1 1.68 1283magn/noentro 1x8 8-sep-02 AB

8 fe1 1.50 1283magn/noentro 2x4 8-sep-02 AB

8 fe1 1.44 1283magn/noentro 4x2 8-sep-02 AB

8 Kabul 0.83 1283magn/noentro 28 MB 20-jun-02 WD

8 Gridur 1.46 1283magn/noentro 19-aug-02 NE

8 Kabul 0.87 2563magn/noentro 160 MB 20-jun-02 WD

8 fe1 0.99 2563magn/noentro 2x4 8-sep-02 AB

8 fe1 0.98 2563magn/noentro 4x2 8-sep-02 AB

8 cetus 0.58 643magn/noentro 4x2 19-aug-07 SS

8 cetus 0.73 2563magn/noentro 4x2,156M 19-aug-07 SS

8 Neolith 0.82 643magn/noentro 4x2 5-dec-07 AB

8 Mhd 1.46 1602

×40 nomag/entro 46 MB 7-oct-02 AB

8 Hwwsx5 0.50 2563convstar 8.6 GB 29-jan-03 WD

8 Neolith 0.444 1283magn/noentro 6-dec-07 AB

8 Ferlin 0.450 6431test/noentro 21-jun-09 AB

8 Ferlin 0.269 643magn/noentro 2-apr-10 AB

8 Ferlin 0.245 1283magn/noentro 2-feb-11 AB

8 nor52 2.00 323magn/noentro 2-dec-09 AB

9 hydra(2) 0.317 723magn/noentro 1x3x3 8-may-16 AB

9 charybdis 0.169 723magn/noentro 1x3x3 8-may-16 AB

9 scylla 0.150 723magn/noentro 1x3x3 8-may-16 AB

12 scylla 0.151 723magn/noentro 1x4x3 8-may-16 AB

12 janus 6.02 722×22 coag/noentro 17-dec-15 AB

16 fe1 1.77 643convstar 9-feb-03 AB

16 copson 0.596 1283geodynamo/ks95 21-nov-03 DM

16 fe1 0.94 1283magn/noentro 4x4 8-sep-02 AB

16 fe1 0.75 1283magn/noentro 4x4/ifc6 9-may-03 AB

16 workq 0.88 1283magn/noentro 4x4/ifc6 21-aug-04 AB

16 giga 0.76 1283magn/noentro 4x4/ifc6 21-aug-04 AB

16 giga2 0.39 1283magn/noentro 4x4/ifc6 20-aug-04 AB

16 giga 0.47 1283chiral 4x4/ifc6 29-may-04 AB

16 giga 0.43 1283nomag/noentro 4x4/ifc6 28-apr-03 AB

16 Mhd 2.03 1283magn/noentro 26-nov-02 AB

16 Mhd 0.64 2563magn/noentro 60 MB 22-may-02 AB

A. Timings 115

16 fe1 0.56 2563magn/noentro 4x4 16-aug-02 AB

16 fe1 6.30 128×256×128 nomag/entro/dust 19-sep-03 AB

16 fe1 1.31 1282

×512 nomag/entro/rad2/ion 4x4 1-nov-03 AB

16 Ukaff 0.61 1283magn/noentro 22-may-02 AB

16 Ukaff 0.64 2563magn/noentro 20-may-02 AB

16 Kabul 0.80 1283magn/noentro 16 MB 20-jun-02 WD

16 Kabul 0.51 2563magn/noentro 9 MB 20-jun-02 WD

16 Gridur 0.81 1283magn/noentro 19-aug-02 NE

16 Gridur 0.66 2563magn/noentro 19-aug-02 NE

16 Sander 0.53 2563magn/noentro 8-sep-02 AB

16 Luci 0.375 1283magn/noentro 28-oct-06 AB

16 Lenn 0.284 1283magn/noentro 8-nov-06 AB

16 Neolith 0.180 2563magn/noentro 6-dec-07 AB

16 Triolith 0.075 1283magn/noentro 2x2x4 1-mar-14 AB

16 Triolith 0.065 1283magn/noentro 1x4x4 1-mar-14 AB

16 Triolith 0.054 2563magn/noentro 1x4x4 1-mar-14 AB

16 Coma 0.603 1283GW/magn/noentro 1x4x4 27-jul-17 SM

24 Gardar 0.44 1282×48 magn/noentro 6-nov-13 AB

24 Summit 0.041 1443magn/noentro 28-jul-17 AB

32 giga? 0.32 2563magn/noentro 13-sep-03 AB

32 Ukaff 0.34 2563magn/noentro 20-may-02 AB

32 Ukaff 0.32 5123magn/noentro 20-may-02 AB

32 Hermit 0.200 256×512×256 spherical conv/magn 1x8x4 22-aug-13 PJK

32 fe1 0.168 5123nomag/noentro 9-oct-02 AB

32 fe1 1.26 642

×256 nomag/entro/rad/ion 7-sep-03 AB

32 Luci 0.182 2563magn/noentro 26-feb-07 AB

32 Lenn 0.147 2563nomag/entro/cool/fo 4x8 8-nov-06 AB

32 Steno 0.076 2563nomag/entro/cool/fo 4x8 20-jun-06 AB

32 Steno 0.081 2563nomag/entro/cool 4x8 20-jun-06 AB

32 Steno 0.085 2563nomag/entro/cool/sh 4x8 20-jun-06 AB

32 Steno 0.235 5122

×256 mag/entro 4x8 9-jul-06 AB

32 Sanss 0.273 128×2562nomag 4x8 3-jul-07 AB

32 Neolith 0.275 1283testﬁeld4 24-oct-08 AB

32 Ferlin 0.556 1283testscalar 7-jan-09 AB

36 Kraken 0.177 192×384×64 magn/noentro 3x6x2 12-jan-12 WL

36 scylla 0.096 723magn/noentro 1x6x6 8-may-16 AB

48 janus 0.028 722∗216 magn/noentro 4x12 28-mar-16 AB

64 Coma 0.573 1283GW/magn/noentro 1x8x8 7-aug-17 SM

64 fe1 0.24 2563magn/noentro 8x8 2-sep-02 AB

64 giga 0.11 2563nomag/noentro 4x16 29-apr-03 AB

64 giga 0.23 2563nomag/noentro/hyp 4x16 8-dec-03 AB

64 fe1 0.164 5123nomag/noentro/hyp 4x16 17-dec-03 AB

64 giga 0.091 5123nomag/noentro/hyp 4x16 17-dec-03 AB

64 giga 0.150 2563magn/noentro 4x16 1-jul-03 AB

64 giga 0.166 5123magn/noentro 64*173MB 10-jul-03 AB

64 Gridur 0.25 2563magn/noentro 19-aug-02 NE

64 Ukaff 0.17 5123magn/noentro 21-may-02 AB

64 Steno 0.075 5123magn/noentro 8x16 19-oct-06 AB

64 Neolith 0.0695 2563magn/noentro 6-dec-07 AB

64 Ferlin 8.51 150×1282Li mechanism 8x8 21-jun-09 AB

64 Ferlin 0.156 2563magn/noentro 8x8 14-jun-09 AB

64 Akka 0.038 2562

×512 magn/noentro 8x8 27-dec-12 AB

64 Triolith 0.0146 2563magn/noentro 1x8x8 1-mar-14 AB

64 Triolith 0.0164 2563magn/noentro 2x4x8 1-mar-14 AB

64 Hermit 0.101 256×512×256 spherical conv/magn 1x8x8 22-aug-13 PJK

64 Sisu 0.00205 256×512×256 spherical conv/magn 1x8x8 22-aug-13 PJK

72 Kraken 0.093 192×384×64 magn/noentro 3x12x2 12-jan-12 WL

72 Kraken 0.151 96×192×16 magn/noentro 6x12 17-jan-12 WL

72 Kraken 0.091 192×384×32 magn/noentro 6x12 17-jan-12 WL

72 Kraken 0.071 384×768×64 magn/noentro 6x12 17-jan-12 WL

116 THE PENCIL CODE

72 Summit 0.0128 5763magn/noentro 7-aug-17 AB

128 fe1 0.44 2563nomag/entro/rad8/ion 4x32 10-mar-04 TH

128 fe1 2.8 5123magn/noentro 16x8 5-sep-02 AB

128 fe1 0.51 5123magn/noentro 8x16 5-sep-02 AB

128 fe1 0.27 5123magn/noentro 4x32 5-sep-02 AB

128 fe1 0.108 5123magn/noentro 4x32/ifc6 5-jan-02 AB

64+64 giga2 0.0600 5123magn/noentro 4x32/ifc6 21-aug-04 AB

128l giga2 0.0605 5123magn/noentro 4x32/ifc6 21-aug-04 AB

128 fe1 0.35 5123magn/noentro 2x64 9-sep-02 AB

128 fe1 0.094 7863magn/noentro 4x32/ifc6 9-sep-02 AB

128 Hermit 0.0532 256×512×256 spherical conv/magn 1x16x8 22-aug-13 PJK

128 Hermit 0.0493 256×512×256 spherical conv/magn 2x8x8 22-aug-13 PJK

128 Sisu 0.00108 256×512×256 spherical conv/magn 1x16x8 22-aug-13 PJK

144 Kraken 0.080 96×192×32 magn/noentro 6x12x2 13-jan-12 WL

144 Kraken 0.058 192×384×64 magn/noentro 6x12x2 17-jan-12 WL

144 Kraken 0.044 384×768×128 magn/noentro 6x12x2 18-jan-12 WL

144 Gardar 2.19 288×1×288 coag43 8x1x18 13-sep-15 AB

144 Summit 0.0064 5763magn/noentro 7-aug-17 AB

192 Janus 0.0123 144×288×72 magn/noentro/sph 1x24x32 24-jul-16 AB

256 Hermit 0.0328 512×1024×512 spherical conv/magn 1x16x16 22-aug-13 PJK

256 Hermit 0.0285 256×512×256 spherical conv/magn 1x16x16 22-aug-13 PJK

256 giga2 0.028 10243magn/noentro 4x64/ifc6 20-aug-04 AB

256 Hermit 0.0262 256×512×256 spherical conv/magn 2x16x8 22-aug-13 PJK

256 Hermit 0.0254 512×1024×512 spherical conv/magn 2x16x8 22-aug-13 PJK

256 Hermit 0.0226 512×1024×512 spherical conv/magn 4x8x8 22-aug-13 PJK

256 Akka 0.0113 5123magn/noentro 16x16 12-jun-11 AB

256 Sisu 0.00618 256×512×256 spherical conv/magn 1x16x16 22-aug-13 PJK

256 Sisu 0.00500 512×1024×512 spherical conv/magn 1x16x16 22-aug-13 PJK

256 Triolith 0.030 2562×512 magn/rad 1x16x16 17-mar-14 AB

256 Triolith 0.0049 2563magn/noentro 1x16x16 1-mar-14 AB

256 Beskow 3.36 1×1×1024 coag43 1x1x256 3-mar-15 AB

288 Gardar 0.042 5762

×288 magn/rad 1x18x16 17-mar-14 AB

288 Kraken 0.0432 192×384×64 magn/noentro 6x12x4 12-jan-12 WL

288 Kraken 0.0447 96×192×64 magn/noentro 6x12x4 13-jan-12 WL

288 Kraken 0.0201 384×768×256 magn/noentro 6x12x4 18-jan-12 WL

288 Janus 0.0360 2883magn/entro/rad 1x16x18 22-feb-16 AB

288 Summit 0.0033 5763magn/noentro 1x16x18 7-aug-17 AB

512 Hermit 0.01717 512×1024×512 spherical conv/magn 1x32x16 22-aug-13 PJK

512 Hermit 0.0166 256×512×256 spherical conv/magn 1x32x16 22-aug-13 PJK

512 Hermit 0.0142 256×512×256 spherical conv/magn 2x16x16 22-aug-13 PJK

512 Hermit 0.01340 512×1024×512 spherical conv/magn 2x16x16 22-aug-13 PJK

512 Hermit 0.01189 512×1024×512 spherical conv/magn 8x8x8 22-aug-13 PJK

512 Hermit 0.01165 512×1024×512 spherical conv/magn 4x16x8 22-aug-13 PJK

512 Akka 0.0081 5123magn/noentro 16x32 10-sep-11 AB

512 Neolith 0.0073 2563magn/noentro 20-nov-09 AB

512 Gardar 0.0035 5123magn/noentro 14-jan-13 AB

512 Lindgren 0.0040 5122

×1024 magn/noentro 16x32 8-jul-12 AB

512 Sisu 0.00446 256×512×256 spherical conv/magn 4x16x8 22-aug-13 PJK

512 Sisu 0.00435 1024×2048×1024 spherical conv/magn 22-aug-13 PJK

512 Sisu 0.00268 512×1024×512 spherical conv/magn 1x32x16 22-aug-13 PJK

576 Kraken 0.0257 192×384×64 magn/noentro 6x24x4 12-jan-12 WL

576 Kraken 0.0317 1922

×64 magn/noentro 122x4 13-jan-12 WL

576 Kraken 0.0116 7682

×256 magn/noentro 122x4 18-jan-12 WL

576 Summit 0.00183 5763magn/noentro 1x24x48 29-jul-17 AB

576 Beskow 0.00174 5763magn/noentro 1x24x48 23-may-16 AB

768 Lindgren 0.0049 256×11522magn/noentro/sph 1x24x32 17-oct-14 SJ

1024 Hermit 0.00943 512×1024×512 spherical conv/magn 1x32x32 22-aug-13 PJK

1024 Hermit 0.00707 512×1024×512 spherical conv/magn 2x32x16 22-aug-13 PJK

1024 Hermit 0.00698 1024×2048×1024 spherical conv/magn 4x16x16 22-aug-13 PJK

1024 Hermit 0.00630 512×1024×512 spherical conv/magn 4x16x16 22-aug-13 PJK

A. Timings 117

1024 Triolith 0.00236 2563magn/noentro 4x16x16 1-mar-14 AB

1024 Triolith 0.00126 5123magn/noentro 2x16x32 1-mar-14 AB

1024 Triolith 0.00129 5123magn/noentro 4x16x16 1-mar-14 AB

1024 Sisu 0.00225 1024×2048×1024 spherical conv/magn 22-aug-13 PJK

1024 Sisu 0.00148 512×1024×512 spherical conv/magn 2x32x16 22-aug-13 PJK

1152 Kraken 0.0212 192×384×64 magn/noentro 12x24x4 13-jan-12 WL

1152 Kraken 0.00856 384×768×128 magn/noentro 12x24x4 17-jan-12 WL

1152 Kraken 0.00549 768×1536×256 magn/noentro 12x24x4 17-jan-12 WL

1152 Lindgren 0.016 5122

×512 magn/rad 1x36x32 17-mar-14 AB

1152 Lindgren 0.0066 11523magn/noentro 1x32x36 25-nov-14 AB

1152 Beskow 0.0055 11523magn/noentro/GW 1x32x36 27-aug-17 AB

1152 Beskow 0.0024 11523magn/noentro 1x32x36 20-jan-15 AB

1152 Beskow 0.00098 11523magn/noentro 1x32x36 18-jan-16 AB-gnu

1152 Beskow 0.00090 11523magn/noentro 1x32x36 30-mar-17 AB

1152 Beskow 0.0060 11523magn/noentro/GW 1x32x36 31-mar-18 AB

1152 Beskow 0.0063 5763magn/entro/rad 1x32x36 17-feb-18 AB

1536 Lindgren 0.00171 5122

×384 magn/noentro 2x32x24 15-jul-13 AB

2048 Hermit 0.00451 1024×2048×1024 spherical conv/magn 2x32x32 22-aug-13 PJK

2048 Hermit 0.00380 512×1024×512 spherical conv/magn 8x16x16 22-aug-13 PJK

2048 Hermit 0.00355 512×1024×512 spherical conv/magn 4x32x16 22-aug-13 PJK

2048 Hermit 0.00350 1024×2048×1024 spherical conv/magn 4x32x16 22-aug-13 PJK

2048 Lindgren 0.00129 5122

×1024 magn/noentro 32x64 20-apr-13 AB

2048 Lindgren 0.00129 10242

×2048 magn/noentro 32x64 31-jul-12 AB

2048 Triolith 9.3×10−45123magn/noentro 4x16x32 1-mar-14 AB

2048 Sisu 0.00120 1024×2048×1024 spherical conv/magn 22-aug-13 PJK

2048 Sisu 9.2×10−4512×1024×512 spherical conv/magn 4x32x16 22-aug-13 PJK

2304 Triolith 1.07×10−35763magn/noentro 4x18x32 1-mar-14 AB

2304 Kraken 0.02267 192×384×64 magn/noentro 12x24x8 13-jan-12 WL

2304 Kraken 0.01233 192×768×64 magn/noentro 12x48x4 13-jan-12 WL

2304 Kraken 0.00300 768×3072×256 magn/noentro 12x48x4 18-jan-12 WL

4096 Hermit 0.00193 1024×2048×1024 spherical conv/magn 4x32x32 22-aug-13 PJK

4096 Triolith 3.6×10−410243magn/noentro 4x32x32 1-mar-14 AB

4096 Triolith 3.8×10−410243magn/noentro 8x16x32 1-mar-14 AB

4096 Triolith 4.2×10−410243magn/noentro 4x16x64 1-mar-14 AB

4096 Lindgren 4.6×10−420483magn/noentro 4x16x64 26-mar-13 AB

4096 Sisu 6.7×10−41024×2048×1024 spherical conv/magn 22-aug-13 PJK

4608 Triolith 7.4×10−45763magn/noentro 8x18x32 1-mar-14 AB

4608 Triolith 2.7×10−411523magn/noentro 4x32x36 1-mar-14 AB

4608 Triolith 3.0×10−411523magn/noentro 4x36x32 1-mar-14 AB

4608 Triolith 3.7×10−411523magn/noentro 4x18x64 1-mar-14 AB

4608 Triolith 2.36×10−423043magn/noentro 2x32x72 1-mar-14 AB

4608 Kraken 0.00764 192×768×128 magn/noentro 12x48x8 13-jan-12 WL

4608 Kraken 0.00144 768×3072×512 magn/noentro 12x48x8 18-jan-12 WL

6144 Lindgren 4.2×10−410243×1536 magn/noentro 4x16x64 21-oct-13 AB

6144 Lindgren 8.9×10−42562magn/noentro/sph 2x48x64 6-jan-15 SJ

8192 Hermit 0.00101 1024×2048×1024 spherical conv/magn 8x32x32 22-aug-13 PJK

8192 Sisu 4.1×10−41024×2048×1024 spherical conv/magn 22-aug-13 PJK

8192 Triolith 1.48×10−420483magn/noentro 4x32x64 1-mar-14 AB

9216 Kraken 0.00485 192×768×256 magn/noentro 24x48x8 13-jan-12 WL

9216 Kraken 0.00158 768×1536×256 magn/noentro 24x48x8 17-jan-12 WL

9216 Kraken 8.0×10−41536×3072×512 magn/noentro 24x48x8 18-jan-12 WL

9216 Lindgren 2.36×10−423043magn/noentro 4x48x48 15-feb-14 AB

9216 Triolith 1.04×10−35763magn/noentro 16x18x32 1-mar-14 AB

9216 Triolith 1.28×10−423043magn/noentro 4x36x64 1-mar-14 AB

9216 Triolith 1.30×10−423043magn/noentro 4x32x72 1-mar-14 AB

16384 Hermit 6.4×10−41024×2048×1024 spherical conv/magn 16x32x32 22-aug-13 PJK

18432 Kraken 0.00316 384×768×256 magn/noentro 24x48x16 13-jan-12 WL

18432 Kraken 8.8×10−4768×1536×512 magn/noentro 24x48x16 17-jan-12 WL

18432 Kraken 4.0×10−41536×3072×1024 magn/noentro 24x48x16 18-jan-12 WL

36864 Kraken 0.0020 384×768×512 magn/noentro 482x16 14-jan-12 WL

118 THE PENCIL CODE

36864 Kraken 4.9×10−415362

×512 magn/noentro 482x16 17-jan-12 WL

36864 Kraken 2.2×10−41536×3072×2048 magn/noentro 24x48x32 18-jan-12 WL

73728 Kraken 0.00121 7682

×512 magn/noentro 482x32 19-jan-12 WL

73728 Kraken 2.9×10−415362

×1024 magn/noentro 482x32 26-jan-12 WL

73728 Kraken 1.2×10−430722

×2048 magn/noentro 482x32 26-jan-12 WL

The machines we have used can be characterized as follows:

Nl3: 500 MHz Pentium III single CPU; RedHat Linux 6.2; 256 MB memory

Nq0: 931 MHz Pentium III single CPU; RedHat Linux 7.3; 0.5 GB memory

Nq[1-4]: 869 MHz Pentium III dual-CPU cluster; RedHat Linux 7.3; 0.77 GB memory

per (dual) node

Nq[5-6]: 1.2 GHz Athlon dual-CPU cluster; RedHat Linux 7.3; 1 GB memory per (dual)

node

Kabul: 1.9 GHz Athlon dual-CPU cluster; 1 GB memory per (dual) node; 256 kB cache

per CPU; Gigabit ethernet; SuSE Linux 8.0; LAM-MPI

Cincinnatus: 1.7 GHz Pentium 4 single CPU; 1 GB memory; 256 kB cache per CPU;

SuSE Linux 7.3

Horseshoe (fe1, giga, and giga2): consists of different subclusters. The old one

(queue name: workq, referred to as fe1) 2.0 GHz Pentium 512 single CPU; 25x 24-

port fast ethernet switches with gigabit ethernet uplink; 1 30-port gigabit ethernet

switch; 1 GB memory. The next generation has gigabit switches directly between

nodes, and 2.6 GHz processors. The third generation (giga2) has 3.2 GHz proces-

sors (most of which have 1 GB, some 2 GB), is organized in 2 blocks interconnected

with 2 Gb links, with 10 Gb uplinks within each block.

Ukaff: SGI Origin 3000; 400 MHz IP35 CPUs; IRIX 6.5; native MPI

Mhd: EV6 Compaq cluster with 4 CPUs per node; 4 GB memory per node (i. e. 1 GB per

CPU) OSF1 4.0; native MPI

Sander and Rasmussen: Origin 3000

Steno 118 node IBM cluster with dual node AMD Opteron processors with 10 Gb in-

ﬁniband network, compiled with pgf90 -fastsse -tp k8-64e (Copenhagen).

Gridur: Origin 3000

Luci: (full name Lucidor) is an HP Itanium cluster, each of the 90 nodes has two 900

MHz Itanium 2 ”McKinley” processors and 6 GB of main memory. The interconnect

is myrinet.

Lenn: (full name Lenngren) is a Dell Xeon cluster with 442 nodes. Each node has two

3.4GHz “Nocona” Xeon processors and 8GB of main memory. A high performance

Inﬁniband network from Mellanox is used for MPI trafﬁc.

Kraken: Cray Linux Environment (CLE) 3.1, with a peak performance of 1.17

PetaFLOP; the cluster has 112,896 cores, 147 TB of memory, in 9,408 nodes. Each

node has two 2.6 GHz six-core AMD Opteron processors (Istanbul), 12 cores, and

16 GB of memory. Connection via Cray SeaStar2+ router.

A. Timings 119

Hermit: Cray XE6 with 7104 2.3 GHz AMD Interlagos 16 core processors (113,664

cores in total), nodes with either 1 or 2 GB of memory per core.

Sisu: Cray XC30 with 1472 2.6 GHz Intel (Xeon) Sandy Bridge 8 core (E5-2670) pro-

cessors (11,776 cores in total), 2 GB of memory per core.

Beskow: Cray XC40 with 2.3 GHz Intel (Xeon) Haswell 16 core (E5-2698v3) processors

(67,456 cores in total), 2 GB of memory per core. Theoretical peak performance 2.43

pﬂops.

Table 8 shows a similar list, but for a few well-deﬁned sample problems. The

svn

check-

in patterns are displayed graphically in Fig 1.

Figure 12: Scaling results on three different machines. The thin straight line denotes perfectly linear

scaling.

5123 gas + 64×106 particles

100 1000 10000

No. of cores

0.001

0.010

0.100

Time per step per point [µs]

NGP+FFT

TSC

NGP

Figure 13: Scaling results of particle-mesh problem on Blue Gene/P on up to 4096 cores. The different

lines denote different particle-mesh schemes (NGP=Nearest Grid Point, TSC=Triangular Shaped Cloud)

and whether self-gravity is included (FFT).

120 THE PENCIL CODE

Strong scaling − Problem size 192 x 384 x 64

100 1000

proc #

0.01

0.10

µs/timestep/point

323

163

Figure 14: Scaling results on Kraken at ﬁxed problem size, for a magnetized disk model in cylindrical

coordinates. The black line shows ideal scaling from 32 cores. The blue line is the best second-order ﬁt to

the data points. A load of 163mesh points per processor marks the best strong scaling.

A.1 Test case

In the following test samples, we run isothermal magnetohydrodynamics in a periodic

domain17. Power spectra are computed during the run, but our current parallelization

of the Fourier transform requires that the meshpoint number is an integer multiple of

the product of processor numbers in the yand zdirections and the product of processor

numbers in the xand ydirections. In addition, the number of processors in one direction

17Run directories are available on http://norlx51.nordita.org/~brandenb/pencil-code/timings/bforced/

102103104105

proc #

0.01

0.10

Wall time (hours)

102103104105

proc #

0.0001

0.0010

0.0100

0.1000

µs/timestep/point

163 p=0.70

323 p=0.85

643 p=0.93

Weak Scaling

Figure 15: Scaling results on Kraken at ﬁxed load per processor, for a magnetized disk model in cylindrical

coordinates. The ﬁgure shows, after determining that 163is the best load per processor for strong scaling,

how far one can push with weak scaling. The scaling index is found to be 0.7 for 163and 0.93 for 643, up

to 73 728 processors.

A.2 Running the code 121

Table 8: Like previous table, but for the versions from the ‘samples’ directory.

proc(s) machine µs

pt step resol. mem./proc when who

conv-slab

1 Mhd 6.45 3234 MB 23-jul-02 wd

1 Cincinnatus 4.82 3233 MB 23-jul-02 wd

1 Cincinnatus 11.6 64314 MB 23-jul-02 wd

1 Cincinnatus 20.8 128393 MB 23-jul-02 wd

1 Kabul 3.91 32323-jul-02 wd

1 Kabul 3.88 64323-jul-02 wd

1 Kabul 4.16 128393 MB 23-jul-02 wd

conv-slab-ﬂat

1 Kabul 3.02 1282

×32 29 MB 23-jul-02 wd

2 Kabul 1.81 1282

×32 18 MB 23-jul-02 wd

4 Kabul 1.03 1282

×32 11 MB 23-jul-02 wd

8 Kabul 0.87 1282

×32 9 MB 23-jul-02 wd

should not be so large that the number of mesh points per processor becomes comparable

to or less than the number of ghost zones (which is 6).

A.2 Running the code

To run the code, get one of the sample run directories, e.g.,

http://norlx51.nordita.org/~brandenb/pencil-code/timings/bforced/512_4x16x32.

The relevant ﬁle to be changed is src/cparam.local

ncpus=2048,nprocx=4,nprocy=16,nprocz=ncpus/(nprocx*nprocy)

nxgrid=512,nygrid=nxgrid,nzgrid=nxgrid

in particular the values of ncpus, nprocx, nprocy, and nxgrid. Once they are chosen, say

make, and submit start run.csh.

A.3 Triolith

On Triolith, strong scaling tests have been performed for three mesh sizes. The time per

time step and mesh point is given for different processor numbers and layouts. Gener-

ally, it is advantageous to keep the number of processors in the xdirection small.

Comments. Although on Triolith the number of processors per node is 16, resolutions

with one or two powers of 3 (such as 576) still work well. Furthermore, the number

of processors above which the scaling becomes poor increases quadratically with the

number of mesh points. This implies that the RAM per processor increases linearly with

the problem size per direction. However, this will not be a limitation, because even for

23043meshes, the required RAM is still below 100 MB.

A.4 Lindgren

On Lindgren, we have performed weak scaling tests and compare with weak scaling

results for Triolith. Triolith is about twice as fast as Lindgren.

122 THE PENCIL CODE

Figure 16: Strong scaling on Triolith (2014).

Figure 17: Comparison Triolith (black, plus signs) and Lindgren (red, triangles). Weak scaling (2014).

A.4 Lindgren 123

Table 9: Triolith timings

proc µs

pt step resol. layout

16 0.075 12832x2x4

16 0.065 12831x4x4

16 0.0544 25631x4x4

64 0.0146 25631x8x8

64 0.0164 25632x4x8

256 0.0049 25631x16x16

512 0.0035 25632x16x16

1024 0.00236 25632x16x32

1024 0.00127 51232x16x32

1024 0.00129 51234x16x16

2048 9.34×10−451234x16x32

2304 0.00107 57634x18x32

4096 3.6×10−4102434x32x32

4096 3.8×10−4102438x16x32

4096 4.2×10−4102434x16x64

4608 7.38×10−457638x18x32

4608 2.66×10−4115234x32x36

4608 3.03×10−4115234x36x32

4608 3.12×10−4115234x18x64

4608 2.36×10−4230432x32x72

8192 1.475×10−4204834x32x64

9216 0.00104 576316x18x32

9216 1.276×10−4230434x36x64

9216 1.30×10−4230434x32x72

Table 10: Lindgren timings

proc µs

pt step resol. layout

1536 0.00171 5122×384 2x32x24

2048 0.00129 5122×1024 1x32x64

2048 0.00129 10242×2048 1x32x64

4096 4.6×10−4204834x16x64

9216 2.36×10−4230434x48x48

124 THE PENCIL CODE

B Coding standard

The numerous elements that make up the PENCIL CODE are written in a consistent

style that has evolved since it was ﬁrst created. Many people have contributed their

knowledge and experience with in this and the result is what we believe is and extremely

readable and manageable code.

As well as improving the readability of the code, by having some naming conventions for

example aids greatly in understanding what the code does.

There is a standard for all aspects of the code, be it Fortran source, shell scripts, Perl

scripts, LaTeX source, Makeﬁles, or otherwise. Where nothing has been explicitly stated

it is recommended that similar existing examples found in the code are used as a tem-

plate.

B.1 File naming conventions

All ﬁles with the exception of the ‘Makefile’s are given lowercase ﬁlenames.

Fortran source ﬁles all have the ‘.f90’ extension. Files that contain ‘non-executable code’

i.e. declarations that are included into other ﬁles are given the extension ‘.h’ and those

that are generated dynamically at compile time have an ‘.inc’ extension.

Fortran source code deﬁning a module is placed in ﬁles whose names begin with the

Fortran module name in all lowercase. Where there exist multiple implementations of

a speciﬁc module the ﬁlenames are extended using and with an underscore ad a brief

name relating to what they do.

Text ﬁles containing parameters to be read by the code at run time are placed in ﬁles

with the extension ‘.in’

B.2 Fortran Code

The code should remain fully compatible with the Fortran90 standard. This ensures that

the code will run on all platforms. Indeed, an important aspect of PENCIL CODE philos-

ophy is to be maximally ﬂexible. This also means that useful non-standard extensions

to the code should be hidden in and be made accessible through suitable non-default

modules.

Fortran is not case-sensitive but in almost all instances we prescribe some form of capi-

talization for readability.

In general all Fortran code including keywords, variable names etc. are written in low-

ercase. Some of the coding standard has already been discussed in Sect. 9.1. Here we

discuss and amplify some remaining matters.

B.2.1 Indenting and whitespace

Whitespace should be removed from the end of lines.

Blank lines are kept to a minimum, and when occurring in subroutines or functions are

replaced by a single ‘!’ in the ﬁrst column.

B.2 Fortran Code 125

Tab characters are not used anywhere in the code. Tab characters are not in fact allowed

by the Fortran standard and compilers that accept them do so as an extension.

All lines are kept to be not more than 80 characters long. Where lines are longer they

must be explicitly wrapped using the Fortran continuation character ‘&’. Longer lines

(up to 132 characters) and additional spaces are allowed in cases where the readability

of the code is enhanced, e.g. when one line is followed by a similar one with minor

differences in some places.

Code in syntactic blocks such as if–endif,do–enddo,subroutine–endsubroutine etc. is

always indented by precisely two spaces. The exception to this is that nested loops where

only the innermost loop contains executable code should be written with the do–enddo

pairs at the same level of indentation,

do n=n1,n2

do m=m1,m2

[...]

enddo

Alternatively nested loops may be written on a single line, i.e.

do n=n1,n2; do m=m1,m2

[...]

enddo; enddo

B.2.2 Comments

Descriptive comments are written on their own lines unless there is a strong reason to do

otherwise. Comments are never indented and the ‘!’ should appear in the ﬁrst column

followed by two spaces and then the text of the comment. Extremely short comments

may follow at the end of a line of code, provided there is space.

Comments also must not exceed the 78 character line length and should be wrapped

onto more lines as needed.

Typically comments should appear with a blank commented line above and below the

wrapped text of the comment.

All subroutine/functions begin with a standard comment block describing what they do,

when and by whom they were created and when and by whom any non-trivial modiﬁca-

tions were made.

Comments should be written in sentences using the usual capitalization and punctua-

tion of English, similar to how text is formatted in an e-mail or a journal article.

For example:

some fortran code

some more fortran code

! A descriptive comment explaining what the following few lines

! of code do.

the fortran code being described

126 THE PENCIL CODE

the fortran code being described

...

! A final detail described here.

the final fortran code

...

Subroutines and functions are started with a comment block describing what they do,

when and by whom they were created and when and by whom any non-trivial modiﬁca-

tions were made. The layout of this comment block is a standard, for example:

!***********************************************************************

subroutine initialize_density(f,lstarting)

! Perform any post-parameter-read initialization i.e. calculate derived

! parameters.

! For compatibility with other applications, we keep the possibility

! of giving diffrho units of dxmin*cs0, but cs0 is not well defined general.

! 24-nov-02/tony: coded

! 1-aug-03/axel: normally, diffrho should be given in absolute units

where dates are written in dd-mmm-yy format as shown and names appearing after the

‘/’ are either the users cvs login name or, where such exists amongst the PENCIL CODE

community, the accepted short form (≈4characters) of the authors name.

B.2.3 Module names

The names of modules are written with initial letter capitalization of each word and the

multiple words written consecutively without any separator.

B.2.4 Variable names

Variable are given short but meaningful names and written in all lowercase. Single

character names are avoided except for commonly used loop indices and the two code

data structures of the PENCIL CODE: ‘f’ the main state array (see 9.3) and ‘p’ the pencil

case structure (see 9.6).

Quantities commonly represented by a particular single character in mathematics are

typically given names formed by repeating the character (usually in lowercase), e.g. the

velocity ubecomes ‘uu’, speciﬁc entropy sbecomes ‘ss’ etc.

Temperature in variable names is denoted with a capital T so as not to be confused

with time as represented by a lowercase t. Note however the since Fortran is not case

sensitive the variables for example ‘TT’ and ‘tt’ are the same so distinct names must

be used. For this reason time is usually represented by a single t contrary to the above

guideline.

B.2 Fortran Code 127

The natural log of a quantity is represented by using adding ‘ln’ to its name, for example

log of temperature would be ‘lnTT’.

There are some standard preﬁxes used to help identify the type and nature of variables

they are as follows:

•i – Denotes integer variables typically used as array indices.

•i– Denotes pencil case array indices.

•idiag – Denotes diagnostic indices.

•l – Denotes logical/boolean ﬂags

•cdt – Denotes timestep constraint parameters.

•unit – Denotes conversion code/physics unit conversion parameters.

B.2.5 Emacs settings

Here are some settings from wd’s ‘~/.emacs’ ﬁle:

;;; ~/.f90.emacs

;;; Set up indentation and similar things for coding the {\sc Pencil Code}.

;;; Most of this can probably be set through Emacs’ Customize interface

;;; as well.

;;; To automatically load this file, put the lines

;;; (if (file-readable-p "~/.f90.emacs")

;;; (load-file "~/.f90.emacs"))

;;; into your ~/.emacs file.

;; F90-mode indentation widths

(setq f90-beginning-ampersand nil) ; no 2nd ampersand at continuation line

(setq f90-do-indent 2)

(setq f90-if-indent 2)

(setq f90-type-indent 2)

(setq f90-continuation-indent 4)

;; Don’t use any tabs for indentation (with TAB key).

;; This is actually already set for F90-mode.

(setq-default indent-tabs-mode nil)

;; Ensure Emacs uses F90-mode (and not Fortran-mode) for F90 files:

(setq auto-mode-alist

(append

’(

("\\.[fF]90$" . f90-mode)

("\\.inc$" . f90-mode)

)

auto-mode-alist))

;; Make M-Backspace behave in Xemacs as it does in GNU Emacs. The default

;; behavior is apparently a long-known bug the fix for which wasn’t

128 THE PENCIL CODE

;; propagated from fortran.el to f90.el.

;; (http://list-archive.xemacs.org/xemacs-patches/200109/msg00026.html):

(add-hook ’f90-mode-hook

(function (lambda ()

(define-key f90-mode-map [(meta backspace)] ’backward-kill-word)

)))

B.3 Other best practices

When implementing IF or SELECT blocks always write code for all cases – including

the default or else case. This should be done even when that code is only a call to raise

an error that the case should not have been reached. If you see a missing case anywhere

then do add it. These failsafes are essential in a large multi-purpose multi-user code

like the PENCIL CODE.

If a case is supposed to do nothing and it may be unclear that the coder has recognized

this fact then make it explicit by adding the default case with a comment like

! Do Nothing. The compiler will clean away any such empty blocks.

B.4 General changes to the code

It is sometimes necessary to do major changes to the code. Since this may af-

fect many people and may even be controversial among the developers, such

changes are restricted to the time of the next Pencil Code User Meeting. Such

meetings are advertised on http://www.nordita.org/software/pencil-code/ under

the news section. Notes about previous such meetings can be found under

http://www.nordita.org/software/pencil-code/UserMeetings/.

Major changes can affect those developers who have not checked in their latest changes

for some time. Before doing such changes it is therefore useful to contact the people who

have contributed to the latest developments on that module. If it is not functional or oth-

erwise in bad shape, it should be moved to ‘experimental’, i.e. one says svn mv file.f90

experimental/file.f90. However, any such directory change constitutes a major change

in itself and should be performed in agreement with those involved in the development.

Otherwise any ﬁle that has been changed in the mean time will end up being outside

revision control, which is to be avoided at all cost.

C. Some speciﬁc initial conditions 129

C Some speciﬁc initial conditions

C.1 Random velocity or magnetic ﬁelds

Obtained with inituu=’gaussian-noise’ (or initaa=’gaussian-noise’). The vector u(or

A) is set to normally distributed, uncorrelated random numbers in all meshpoints for

all three components. The power spectrum of u(A) increases then quadratically with

wavenumber k(without cutoff) and the power spectrum of ω(or B) increases like k4.

Note that a random initial condition contains signiﬁcant power at the Nyquist frequency

(kNy =π/N, where Nis the number of mesh points). In a decay calculation, because of

the discretization error, such power decays slower than it ought to; see Fig. 18, where

we show the evolution for a random initial velocity ﬁeld for 643meshpoints, ν= 5 ×10−2

(fairly large!), and nfilter=30.

It is clearly a good idea to ﬁlter the initial condition to prevent excess power at kNy. On

the other hand, such excess power is weak by comparison with the power at the energy

carrying scale, so one does not see it in visualizations in real space. Furthermore, as seen

from Fig. 18, for k < kNy/2the power spectra for ﬁltered and unﬁltered initial conditions

is almost the same.

Figure 18: Velocity power spectra at three different times with and without ﬁltering of the initial condi-

tion.

C.2 Turbulent initial with given spectrum

The most general procedure for producing an initial condition with a turbulent spec-

trum is inituu=’power_randomphase_hel’, which allows one to set two different slopes,

together with an exponential cutoff as well as a Gaussian peak within the spectrum. By

default, the ﬁeld is solenoidal unless one puts lskip_projection=.true. and can have

fractional helicity by setting relhel_uu to a value between −1and 1. By default it is 0,

which means it is nonhelical.

130 THE PENCIL CODE

The spectral indices

initpower

and

initpower2

refer to energy spectral indices. By de-

fault,

initpower2=-5/3

, corresponding to a Kolmogorov spectrum. For a delta-correlated

spectrum, we have to put

initpower=2

, corresponding to a k2energy spectrum for ki-

netic energy. This would be suitable for the subinertial range from k= 1 to k=kp

(corresponding to the variable

kpeak

cutoff=0

, no cutoff will be imposed. Otherwise, the spectrum will be multiplied by an

exponential function with exp(−k2n), where n=’ncutoff=1’ by default.

Example, for

ampluu=1e-1

initpower=4.

, and

kpeak=3.

, we get

urms=3.981E-01

when

relhel uu=1

and

urms=3.981E-01

when

relhel uu=0

and

urms=5.560E-01

when

relhel -

uu=1

. The

urms

values scale linearly with

ampluu

and for

initpower=2

also approxi-

mately linearly with

kpeak

. For the magnetic ﬁeld, we initialize the magnetic vector

potential, so to get a k4spectrum, we have to put

initpower aa=2.

Everything else is

analogous; see, e.g.,

&hydro_init_pars

inituu=’power_randomphase_hel’, ampluu=1e-1, initpower=4., kpeak=3.

relhel_uu=0., cutoff=30.

&magnetic_init_pars

initaa=’power_randomphase_hel’, amplaa=1e-1, initpower_aa=2., kpeak_aa=3.

relhel_aa=0., cutoff_aa=30.

for which we get

urms=3.981E-01

and

brms=3.871E-01

C.3 Beltrami ﬁelds

Obtained with inituu=’Beltrami-z’ or initaa=’Beltrami-z’.

A= (cos z, sin z, 0),or u= (cos z, sin z, 0) (126)

C.4 Magnetic ﬂux rings: initaa=’fluxrings’

This initial condition sets up two interlocked thin magnetic tori (i. e. thin, torus-shaped

magnetic ﬂux tubes). One torus of radius Rlying in the plane z= 0 can be described in

cylindrical coordinates, (r, ϕ, z), by the vector potential

A= Φm



−θ(r−R)δ(z)

,(127)

resulting in a magnetic ﬁeld

B= Φm



δ(r−R)δ(z)

0

.(128)

Here Φmis the magnetic ﬂux through the tube, θ(x)denotes the Heaviside function, and

δ(x) = θ′(x)(129)

C.5 Vertical stratiﬁcation 131

is Dirac’s delta function.

Any smoothed versions of θ(x)and δ(x)will do, as long as the consistency condition (129)

is satisﬁed. E. g. the pairs

δε(x) = 1

√2πε2e−x2

2ε2, θε(x) = 1

21 + erf x

√2ε(130)

δε(x) = 1

2ε

cosh2x

, θε(x) = 1

21 + tanh x

ε(131)

are quite popular. Another possibility is a constant or box-like proﬁle with

δε(x) = 1

2εθ(|x| − ε), θε(x) = 1

2{1 + max[−1,min(x/ε),1]}(132)

Note, however, that the Gaussian proﬁle (130) is the only one that yields a radially

symmetric (with respect to the distance from the central line of the torus) magnetic ﬁeld

proﬁle Bϕ=Bφ(p(r−R)2+z2)if εis sufﬁciently small.

In Cartesian coordinates, the vector potential (127) takes the form

A= Φm





−θpx2+y2−Rδ(z)



.(133)

C.5 Vertical stratiﬁcation

Gravity, g=−∇Φ, is speciﬁed in terms of a potential Φ. In slab geometry, Φ = Φ(z), we

have g= (0,0, gz)and gz=−dΦ/dz.

Use

grav proﬁle

=’const’ together with

gravz

=−1to get

Φ = (z−z∞)(−gz),(−gz)>0.(134)

Use

grav proﬁle

=’linear’ to get

Φ = 1

2(z2−z2

∞)ν2

g, gz=−ν2

gz(135)

where νgis the vertical epicyclic frequency. For a Keplerian accretion disc, νg=Ω. For

galactic discs, νg= 0.5Ωis representative of the solar neighborhood.

The value of z∞is determined such that ρ=ρ0and c2

s=c2

s0 at z=zref . This depends on

the values of γand the polytropic index m(see below).

C.5.1 Isothermal atmosphere

Here we want cs=cs0 =const. Using initlnrho=’isothermal’ means

ln ρ

ρ0

=−γΦ

.(136)

The entropy is then initialized to

= (γ−1) Φ

.(137)

In order that ρ=ρ0and c2

s=c2

s0 at z=zref , we have to choose z∞=zref .

132 THE PENCIL CODE

C.5.2 Polytropic atmosphere

For a polytropic equation of state, p=KρΓ, where generally Γ6=γ, we can write

−∇h+T∇s=−1

ρ∇p=−∇ΓK

Γ−1ρΓ−1≡ −∇˜

h, (138)

where we have introduced a pseudo enthalpy ˜

has

h=ΓK

Γ−1ρΓ−1=1−1

γ1−1

Γh . (139)

Obviously, for Γ = γ, the pseudo enthalpy ˜

his identical to hitself. Instead of specifying

Γ, one usually deﬁnes the polytropic index m= 1/(Γ−1). Thus, Γ = 1 + 1/m, and

h= (m+1) 1−1

γh(140)

This is consistent with a ﬁxed entropy dependence, where sonly depends on ρlike

=Γ

γ−1ln ρ

ρ0

,(141)

and implies that

ln c2

= (Γ−1) ln ρ

ρ0

.(142)

For hydrostatic equilibrium we require ˜

h+ Φ = ˜

h0=const. For gravity potentials that

vanish at inﬁnity, we can have ˜

h06= 0, i.e. a ﬁnite pseudo enthalpy at inﬁnity. For gz=−1

or gz=−z, this is not the case, so we put ˜

h0= 0, and therefore ˜

h=−Φ. Using c2

s= (γ−1)h

together with (140) we ﬁnd

s=−γ

m+1 Φ.(143)

In order that ρ=ρ0and c2

s=c2

s0 at z=zref , we have to choose (remember that gzis

normally negative!)

z∞=zref + (m+1) c2

γ(−gz)for

grav proﬁle

=’const’,(144)

and

∞=z2

ref + (m+1) c2

2γν2

for

grav proﬁle

=’linear’.(145)

Thus, when using initlnrho=’polytropic_simple’ we calculate

ln c2

= ln −γΦ

(m+1)c2

s0 (146)

and so the stratiﬁcation is given by

ln ρ

ρ0

=mln c2

=Γ

γ−1mln c2

.(147)

C.5 Vertical stratiﬁcation 133

C.5.3 Changing the stratiﬁcation

Natural: measure length in units of c2

s0/gz. Can increase stratiﬁcation by moving ztop

close to z∞or, better still, keeping ztop = 0 and moving zbot → −∞. Disadvantage: in the

limit of weak stratiﬁcation, the box size will be very small (in nondimensional units).

Box units: measure length in units of d. Can increase stratiﬁcation by increasing gzto

gmax, which can be obtained by putting ztop =z∞in (144), so

gmax =m+1

ztop −zref

.(148)

For m= 1,γ= 5/3,ztop = 1, and zref = 0, for example, we have gmax = 6/5 = 1.2.

Gravitational box units: measure speed in units of √gzd. The limit of vanishing stratiﬁ-

cation corresponds to cs0 → ∞. This seems optimal if we want to approach the Boussi-

nesq case.

In Hurlburt et al. (1984), zincreased downward and the atmosphere always terminated

at z= 0. In order to reproduce their case most directly, we put z∞= 0 and consider only

negative values of z. To reproduce their case with a density stratiﬁcation of 1:1.5, we

place the top of the model at z=−2and the bottom at z=−3. In addition, the reference

height, zref , is chosen to be at the top of the box, i.e. zref =−2. From Eq. (144) we have

s0 =γ(−gz)(−zref )/(m+ 1). Using (−gz) = 1 and m= 1 we ﬁnd c2

s0 =γ, so cs0 = 1.291 (for

γ= 5/3). Values for other combinations are listed in Table 11.

Table 11: Correspondence between density contrast, top and bottom values of z, and cs0 for (−gz) = 1,

m= 1, and γ= 5/3.

ρbot/ρtop zbot ztop cs0

1.5 3 2 1.291

3 1.5 0.5 0.645

6 1.2 0.2 0.408

11 1.1 0.1 0.289

21 1.05 0.05 0.204

C.5.4 The Rayleigh number

In Ref. [11] the Rayleigh number is deﬁned as

Ra = gd4

ν χ −ds/cp

dzhydrostat

,(149)

where the (negative) entropy gradient was evaluated in the middle of the box for the

associated hydrostatic reference solution, and χ=K/(ρcp)and either ν=ν(if νwas

assumed constant) or ν=µ/ρ (if µwas assumed constant). Note that ρis the average

mass in the box per volume, which is conserved. For a polytrope we have

−ds/cp

dzhydrostat

=1−(m+ 1) 1−1

γ 1

z∞−zm

,(150)

where zm= (z1+z2)/2. This factor was also present in the deﬁnition of Hurlburt et al.

[22], but their deﬁnition differs slightly from Eq. (149), because they normalized the

134 THE PENCIL CODE

density not with respect to the average value (which is constant for all times), but with

respect to the value at the top of the initial hydrostatic solution. Since the Rayleigh

number is proportional to ρ2, their deﬁnition included the extra factor [(z∞−zm)/d]2.

Therefore

RaHTM =z∞−zm

d2mρtop

ρ2

Ra (151)

In the ﬁrst model of Hurlburt et al. (1984), the Rayleigh number, RaHTM, was chosen to

be 310 times supercritical, and the critical Rayleigh number was around 400, so RaHTM =

1.25 ×105. In their model the density contrast was 1:1.5 and m= 1. This turns out to

correspond to Ra = 4.9×104,Fbot = 0.0025, and K= 0.002.

Another model that was considered by Hurlburt & Toomre (1988) had RaHTM = 105,

a density contrast of 11, and had a vertical imposed magnetic ﬁeld (Chandrasekhar

number Q= 72). This corresponds to Ra = 3.6×108,K= 0.0011,Fbot = 0.0014.

C.5.5 Entropy boundary condition

This discussion only applies to the case of convection in a slab. A commonly used lower

boundary condition is to prescribe the radiative ﬂux at the bottom, i.e. Fbot =−KdT/dz.

Assuming that the density in the ghost zones has already been updated, we can calculate

the entropy gradient from

Fbot =−K

γ−1(γ−1)d ln ρ

dz+γds/cp

dz,(152)

which gives

ds/cp

dz=−γ−1

γcp

Fbot

Kc2

+d ln ρ

dz(153)

for the derivative of the entropy at the bottom. This is implemented as the ‘c1’ boundary

condition at the bottom.

C.5.6 Temperature boundary condition at the top

In earlier papers the temperature at the top was set in terms of the quantity ξ0, which

is the ratio of the pressure scale height relative to the depth of the unstable layer. Ex-

pressed in terms of the sound speed at the top we have

s,top =γξ0gd. (154)

s,bot =ξ0+1

m+ 1γgd. (155)

C.6 Potential-ﬁeld boundary condition

The ‘pot’ [or currently rather the ‘pwd’] boundary condition for the magnetic vector poten-

tial implements a potential-ﬁeld boundary condition in zfor the case of an x-y-periodic

box. In this section, we discuss the relevant formulas and their implementation in the

PENCIL CODE.

C.6 Potential-ﬁeld boundary condition 135

Table 12: Correspondence between ξ0and c2

s,bot in single layer polytropes.

ξ0c2

s,bot

10.00 17.500

0.20 1.167

0.10 1.000

0.05 0.917

0.02 0.867

If the top boundary is at z= 0, the relevant potential ﬁeld for z > 0is given by

Ax(kx, ky, z) = Cx(kxy)e−κz ,(156)

Ay(kx, ky, z) = Cy(kxy)e−κz ,(157)

Ax(kx, ky, z) = Cz(kxy)e−κz ,(158)

where

Ai(kx, ky, z)≡Ze−ikxy ·xAi(x, y, z)dx dy (159)

is the horizontal Fourier transform with kxy ≡(kx, ky,0), and k≡ |kxy|. Note that this im-

plies a certain gauge and generally speaking the zdependence in Eq. (158) is completely

arbitrary, but the form used here works well in terms of numerical stability.

At the very boundary, the potential ﬁeld (156)–(158) implies

∂˜

∂z +κ˜

A= 0 ,(160)

and, due to natural continuity requirements on the vector potential, these conditions

also hold for the interior ﬁeld at the boundary.

Robin boundary conditions and ghost points To implement a homogeneous Robin

boundary condition, i. e. a condition of the form

dz +κf = 0 (161)

using ghost points, we ﬁrst write it as

dz (f eκz) = 0 (162)

and implement this as symmetry condition for the variable φ(z)≡f(z)eκz:

φN−j=φN+j, j = 1,2,3(163)

(where zNis the position of the top boundary and zN+1, . . . are the boundary points). In

terms of f, this becomes

fN+j=fN−je−κ(zN+j−zN−j).(164)

Note that although the exponential term in Eq. (164) looks very much like the exterior

potential ﬁeld (156)–(158), our ghost-zone values do not represent the exterior ﬁeld –

they are rather made-up values that allow us to implement a local boundary condition

at z= 0.

136 THE PENCIL CODE

C.7 Planet solution in the shearing box

In order to test the setup for accretion discs and the sliding periodic shearing sheet

boundary condition, a useful initial condition is the so-called planet solution of Good-

man, Narayan, & Goldreich [19].

Assume s= 0 (isentropy), so the equations in 2-D are

uxux,x + (u(0)

y+uy)ux,y = 2Ωuy−h,x (165)

uxuy,x + (u(0)

y+uy)uy,y =−(2 −q)Ωux−h,y (166)

where u(0)

y=−qΩx. Express uin terms of a stream function, so u=∇ × (ψˆ

z), or

ux=ψ,y, uy=−ψ,x.(167)

Ansatz for enthalpy

h=1

2δ2Ω2(R2−x2−ǫ2y2−z2/δ2)(168)

ψ=−1

2σΩ(R2−x2−ǫ2y2)−1

2qΩx2(169)

This implies

ux=σΩǫ2y, uy= (q−σ)Ωx (170)

and ux,x =uy,y = 0. Inserting into Eqs (165) and (166) yields

(−q+q−σ)σǫ2= 2(q−σ) + δ2(171)

σ(q−σ) = −(2 −q)σ+δ2(172)

where we have already canceled common Ω2factors in both equations and common ǫ2

factors in the last equation. Simplifying both equations yields

−σ2ǫ2= 2(q−σ) + δ2(173)

−σ2=−2σ+δ2(174)

The second equation yields

δ2= (2 −σ)σ(175)

and subtracting the two yields

σ2= 2q/(1 −ǫ2)(176)

Table 13: Dependence of ǫand δon ǫ.

ǫ σ δ

0.1 1.74 0.67

0.2 1.77 0.64

0.3 1.82 0.58

0.4 1.89 0.46

0.48 1.97 0.22

0.5 2 0

D. Some speciﬁc boundary conditions 137

D Some speciﬁc boundary conditions

In this section, we formulate and discuss the implementation of some common boundary

conditions in spherical and cylindrical coordinates.

D.1 Perfect-conductor boundary condition

This is a popular boundary condition for the magnetic ﬁeld; it implies that

Bn= 0 (177)

and

Et= 0 (178)

on the boundary, where the subscript ndenotes the normal component, and Etdenotes

the tangential components of the electric ﬁeld.

In Cartesian geometry, these conditions can be implemented by setting the two tangen-

tial components of the vector potential Ato zero on the boundary. It is easy to see that

this also works in arbitrary curvilinear coordinates.

In particular, for spherical coordinates on a radial boundary we must have

rsin θ Br=∂θ(sin θ Aφ)−∂φAθ= 0 .(179)

This can be achieved by setting

Aφ=Aθ= 0 (180)

everywhere on the boundary. Note that this does not impose any condition on the radial

component of the vector potential.

Next, in spherical coordinates on a boundary with constant θ, we must have

Bθ=1

rsin θ∂φAr−1

r∂r(rAφ) = 0 .(181)

Again this can be achieved by Ar=Aφ= 0.

D.2 Stress-free boundary condition

On an impenetrable, stress-free boundary, we have

un= 0 ,(182)

and the shear stress components Snt must vanish for any tangential direction t. At the

radial boundary, the relevant components of the strain tensor (required to vanish at the

boundary) are:

Srθ =1

r∂θur+r∂ruθ

r,(183)

Srφ =1

rsin θ∂φur+r∂ruφ

r.(184)

Both of them vanish if we require

ur= 0 , ∂r(uθ/r) = 0 , ∂r(uφ/r) = 0 .(185)

138 THE PENCIL CODE

We implement this by requiring urto be antisymmetric and uθ/r and uφ/r to be symmet-

ric with respect to the boundary.

The more general condition

rα∂r(uθ/rα) = ∂ruθ−α

ruθ= 0 (186)

(where αis a constant) can be implemented by requiring uθ/rαto be symmetric.

At a boundary θ=const, the stress-free boundary condition will take the form

Srθ =1

r∂θur+r∂ruθ

r= 0 ,(187)

Sθφ =1

rsin θ∂φuθ+ sin θ ∂θuφ

rsin θ= 0 .(188)

With uθ= 0, the ﬁrst condition gives ∂θur= 0, i.e. we require urto be symmetric with

respect to the boundary. The second condition requires

sin θ

r∂θuφ

sin θ= 0 (189)

and is implemented by requiring uφ/sin θto be symmetric.

D.3 Normal-ﬁeld-radial boundary condition

While unphysical, this boundary condition is often used as a cheap replacement for a

potential-ﬁeld condition for the magnetic ﬁeld. It implies that the two tangential com-

ponents of the magnetic ﬁeld are zero at the boundary, while the normal component is

left unconstrained.

At a radial boundary, this gives:

Bθ=1

rsin θ∂φAr−1

r∂r(rAφ) = 0 ,(190)

Bφ=1

r∂r(rAθ)−1

r∂θAr= 0 .(191)

Which are satisﬁed by setting

Ar= 0 , ∂r(rAθ) = 0 , ∂r(rAφ) = 0 ,(192)

and these are implemented by requiring Arto be antisymmetric, and rAθand rAφto be

symmetric.

On a boundary θ=const, we have

rsin θ Br=∂θ(sin θ Aφ)−∂φAθ= 0 ,(193)

rBφ=∂r(rAθ)−∂θAr= 0 (194)

which can be achieved by setting

∂θAr= 0 , Aθ= 0 , ∂θ(sin θ Aφ) = 0 .(195)

We thus require Arand sin θ Aφto be symmetric, and Aθto be antisymmetric.

E. High-frequency ﬁlters 139

E High-frequency ﬁlters

Being high order, PENCIL CODE has much reduced numerical dissipation. In order to

perform inviscid simulations, high-frequency ﬁlters can be used to provide extra dissi-

pation for modes approaching the Nyquist frequency. Usual Laplacian viscosity ν∇2uis

equivalent to a multiplication by k2in Fourier space, where kis the wavenumber. An-

other tool is hyperviscosity, which replaces the k2dependency by a higher power-law, kn,

n>2. The idea behind it is to provide large dissipation only where it is needed, at the grid

scale (high k), while minimizing it at the largest scales of the box (small k). In principle,

one can use as high nas desired, but in practice we are limited by the order of the code.

A multiplication by knis equivalent to an operator ∇nin real space. As PENCIL CODE

is of sixth order, three ghost cells are available in each direction, thus the sixth-order

derivative is the highest we can compute. The hyperdissipation we use is therefore ∇6,

or k6is Fourier space. Figure 19 illustrates how such tool maximizes the inertial range

of a simulation.

Simpliﬁed hyperdiffusivity has been implemented for many dynamical variables and

can be found in the respective modules. A strict generalization of viscosity and resistivity

to higher order is implemented in the modules ‘hypervisc_strict_2nd’ and ‘hyperresi_-

strict_2nd’.

Hyperdiffusivity is meant purely as a numerical tool to dissipate energy at small scales

and comes with no guarantee that results are convergent with regular second order

dissipation. See Haugen & Brandenburg (2004) for a discussion. In fact, large-scale dy-

namo action is known to be seriously altered in simulations of closed systems where

magnetic helicity is conserved: this results in prolonged saturation times and enhanced

saturation amplitudes (Brandenburg & Sarson 2002).

E.1 Conservative hyperdissipation

It is desirable to have this high-frequency ﬁlter obeying the conservation laws. So, for

density we want a mass conserving term, for velocities we want a momentum conserving

term, for magnetic ﬁelds we want a term conserving magnetic ﬂux, and for entropy we

want an energy conserving term. These enter as hyperdiffusion, hyperviscosity, hyper-

resistivity, and hyper heat conductivity terms in the evolution equations. To ensure con-

servation under transport, they must take the form of the divergence of the ﬂux Jof the

quantity ψ, so that Gauss theorem applies and we have

∂ψ

∂t +∇·J= 0 (196)

For density, the ﬂow due to mass diffusion is usually taken as the phenomenological

Fick’s Law

J=−D∇ρ(197)

i.e., proportional to the density gradient, in the opposite direction. This leads to the

usual Laplacian diffusion

∂ρ

∂t =D∇2ρ(198)

140 THE PENCIL CODE

Laplacian vs hyper dissipation

0.5 1.0 1.5 2.0

0.0

0.5

1.0

1.5

2.0

0.5 1.0 1.5 2.0

−4

−2

Dn∇2nψ

n=1

n=3

1 10 100

10−12

10−10

10−8

10−6

10−4

10−2

100

k2n Dn|ψ|

Figure 19: Dissipation acting on a scalar ﬁeld ψ, for n=1 (Laplacian dissipation) and n=3 (third-order

hyperdissipation). The ﬁeld is initially seeded with noise (upper panel). For n=3 the large scale is not

affected as much as in the n=1 case, which is seen by the larger wiggling of the latter in the middle panel.

In Fourier space (lower panel) we see that near the grid scale both formulations give strong dissipation.

It also illustrates that at the large scales (k≃1), the effect of n=3 is indeed negligible.

under the assumption that the diffusion coefﬁcient Dis isotropic. Higher order hyper-

diffusion of order 2ninvolves a generalization of Eq. (197), to

J(n)= (−1)nD(n)∇2n−1ρ . (199)

In our case, we are interested in the case n= 3, so that the hyperdiffusion term is

∂ρ

∂t =D(3)∇6ρ. (200)

The hyperdiffusion coefﬁcient D(3) can be calculated from Dassuming that at the

Nyquist frequency the two formulations (198) and (200) yield the same quenching. Con-

sidering a wave as a Fourier series in one dimension (x), one element of the series is

expressed as

ψk=Aei(kx+ωt)(201)

E.2 Hyperviscosity 141

Plugging it into the second order diffusion equation (198) we have the dispersion con-

dition iω =−Dk2. The sixth order version (200) yields iω =−D(3)k6. Equating both

we have D(3) =Dk−4. This condition should hold at the grid scale, where k=π/∆x,

therefore

D(3) =D∆x

π4

(202)

For the magnetic potential, resistivity has the same formulation as mass diffusion

∂A

∂t =−η∇ × B=η∇2A,(203)

where we used the Coulomb gauge ∇·A= 0. The algebra is the same as above, also

yielding η(3) =η(∆x/π)4. For entropy, the heat conduction term is

∂S

∂t =1

ρT ∇·(K∇T),(204)

and requiring that Kbe constant, we substitute it by

∂S

∂t =K(3)

ρT ∇6T. (205)

also with K(3) =K(∆x/π)4.

E.2 Hyperviscosity

Viscosity has some caveats where subtleties apply. The difference is that the momentum

ﬂux due to viscosity is not proportional to the velocity gradient, but to the rate-of-strain

tensor

Sij =1

2∂ui

∂xj

+∂uj

∂xi−2

3δij∇·u,(206)

which only allows the viscous acceleration to be reduced to the simple formulation ν∇2u

under the condition of incompressibility and constant dynamical viscosity µ=νρ. Due

to this, the general expression for conservative hyperviscosity involves more terms. In

some cases, it is no great overhead, but for others, simpler formulations can be applied.

E.2.1 Conservative case

In the general case, the viscous acceleration is

fvisc =ρ−1∇·(2ρνS)(207)

So, for the hyperviscous force, we must replace the rate-of-strain tensor by a high order

version

f(hyper)

visc =ρ−1∇·2ρνnS(n)(208)

where the nth-order rate of strain tensor is

S(n)= (−∇2)n−1S.(209)

142 THE PENCIL CODE

For the n= 3 case it is

S(3)

ij =1

2∂5uj

∂xi5+∂4

∂xi4∂ui

∂xj−1

∂4

∂xi4(∇·u).(210)

Plugging it into Eq. (208), and assuming µ3=ρν3= const

f(hyper)

visc =ν3∇6u+1

3∇4(∇(∇·u)).(211)

For ν3= const, we have to take derivatives of density as well

f(hyper)

visc =ν3∇6u+1

3∇4(∇(∇·u)) + 2S(3) ·∇ln ρ(212)

E.2.2 Non-conservative cases

Equations (211) and (212) explicitly conserve linear and angular momentum. Although

desirable properties, such expressions are cumbersome and numerically expensive, due

to the fourth order derivatives of ∇(∇·u).

This term, however, is only important when high compressibility is present (since it

depends on the divergence of u). In practice we drop this term and use a simple hyper-

viscosity

fvisc =(ν3∇6uif µ= const

ν3∇6u+ 2S(3) ·∇ln ρif ν= const (213)

Notice that this can indeed be expressed as the divergence of a simple rate-of-strain

tensor

S(3)

ij =∂5ui

∂xj5,(214)

so it does conserve linear momentum. It does not, however, conserve angular momen-

tum, since the symmetry of the rate-of-strain tensor was dropped. Thus, vorticity sinks

and sources may be spuriously generated at the grid scale.

A symmetric tensor can be computed, that conserves angular momentum and can be

easily implemented

Sij =1

2∂5ui

∂xj5+∂5uj

∂xi5(215)

This tensor, however, is not traceless, and therefore accurate only for weak compressibil-

ity. It should work well if the turbulence is subsonic. Major differences are not expected,

since the spectral range in which hyperviscosity operates is very limited: as a numerical

tool, only its performance as a high-frequency ﬁlter is needed. This also supports the

usage of the highest order terms only, since these are the ones that provide quenching

at high k. Momentum conservation is a cheap bonus. Angular momentum conservation

is perhaps playing it too safe, at great computational expense.

E.2 Hyperviscosity 143

E.2.3 Choosing the coefﬁcient

When changing the resolution, one wants to keep the grid Reynolds number, here de-

ﬁned as

Regrid =urms νnk2n−1

Ny (216)

approximately constant. Here, kNy =π/δx is the Nyquist wavenumber and δx is the

mesh spacing. Thus, when doubling the number of meshpoints, we can decrease the

viscosity by a factor of about 25= 32 (Haugen & Brandenburg 2004). This shows that

hyperviscosity can allow a dramatic increase of the Reynolds number based on the scale

of the box.

By choosing

idiff=’hyper3 mesh’

in density_run_pars the hyperdiffusion for density is

being set automatically in a mesh-independent way. A hyper-mesh Reynolds number of

30 corresponds to a coefﬁcient

diffrho hyper3 mesh=2

maxadvec

is about 1, but in

practice we need a bit more (5 is currently the default).

E.2.4 Turbulence with hyperviscosity

When comparing hyperviscous simulations with non-hyperviscous ones, it turns out that

the Reynolds number at half the Nyquist frequency is usually in the range 5–7, i.e.

Rehalf−grid =urms νn(kNy/2)2n−1≈5–7 (217)

The following table gives some typical values used in simulations with forcing wavenum-

ber kf= 1.5and a forcing amplitude of f0= 0.02. If hyperdiffusion D3is used in the

continuity equation, the corresponding values are about 30 times smaller than those of

ν3; see Table 14.

Table 14: Empirical values of viscosity and hyperviscosity, as well as hyperdiffusion for density, at differ-

ent numerical resolution, for simulations with forcing wavenumber kf= 1.5and a forcing amplitude of

f0= 0.02 in a 2πperiodic domain. In all cases the half-mesh Reynolds number is about 5–7. For compar-

ison, estimates of the numerical 4th order hyperdiffusion resulting from a third order time step are give

for two values of the CFL parameter.

N ν1ν2ν3D3κCFL=0.4

2κCFL=0.9

16 1×10−23×10−42×10−56×10−77×10−41×10−4

32 5×10−34×10−56×10−72×10−81×10−62×10−5

64 2×10−35×10−62×10−86×10−10 2×10−73×10−6

128 1×10−36×10−76×10−10 2×10−11 3×10−84×10−7

256 5×10−48×10−82×10−11 6×10−13 4×10−95×10−8

512 2×10−41×10−86×10−13 2×10−14 5×10−10 6×10−9

1024 1×10−41×10−92×10−14 6×10−16 6×10−11 8×10−10

For comparison, we give in Table 14 estimates of the numerical 4th order hyperdiffusion

resulting from a third order time step, for which we have

κCFL

2=1

24urms (CCFLδx)3(218)

where CCFL is the CFL parameter which is either 0.4 in the conservative case or 0.9 in

the more progressive case.

144 THE PENCIL CODE

E.3 Anisotropic hyperdissipation

As we want quenching primarily at the Nyquist frequency, hyperdissipation depends

intrinsically on the resolution, according to Eq. (202). Because of this, isotropic hyper-

dissipation only gives equal quenching in all spatial directions if ∆x=∆y=∆z, i.e., if the

cells are cubic. For non-cubic cells, anisotropic dissipation is required as different direc-

tions may be better/worse sampled, thus needing less/more numerical smoothing. Such

generalization is straightforward. For that, we replace Eq. (199) by

J=Dx

∂5ρ

∂x5, Dy

∂5ρ

∂y5, Dz

∂5ρ

∂z5,(219)

so that different diffusion operates in different directions. Since Dx,Dyand Dzare con-

stants, the divergence of this vector is

∇·J=Dx

∂6ρ

∂x6+Dy

∂6ρ

∂y6+Dz

∂6ρ

∂z6.(220)

The formulation for resistivity and heat conductivity are strictly the same. For viscosity

it also assumes the same form if we consider the simple non-conservative rate-of-strain

tensor (214).

Mathematically, these operations can be written compactly by noticing that the coefﬁ-

cients in Eq. (220) transform like diagonal tensors χ(3)

ij =χ(3)

kδijk, where δijk is the unit

diagonal third order tensor, χ(3) is the vector containing the dissipative coefﬁcients (dif-

fusion, viscosity, resistivity, or heat conductivity) in x,y, and z, and summation over

repeated indices applies.

Therefore, for a scalar quantity ψ(density, any of the three components of the velocity

or magnetic potential), we can write

∂ψ

∂t =−χ(3)

ij ∂i∂5

jψ=−X

χ(3)

∂6

∂x6

ψ. (221)

E.4 Hyperviscosity in Burgers shock

Figure 20: Left: Burgers shock from teach/PencilCode/material/BurgersShock (in the teaching material)

with −20 ≤x≤20,nx= 64 mesh points, ux=∓1on the two ends, ν= 0.4and either ν3= 0 (solid line)

or ν3= 0.05 (dashed line). Right: similar to the left hand side, but with ν= 0 and ν3= 0.05 (dashed line),

compared with the case ν= 0.4and ν3= 0 (solid line).

E.4 Hyperviscosity in Burgers shock 145

Hyperviscosity has the unfortunate property of introducing (numerically stable) wiggles,

even if one just adds a little bit of hyperviscosity to a run with normal viscosity; see left

hand side of Fig. 20. Running with just hyperviscosity give strong wiggles.

146 THE PENCIL CODE

F Special techniques

F.1 After changing REAL PRECISION

To continue working in double precision (REAL_PRECISION=double), you just say lread_-

from_other_prec=T in run_pars. Afterwards, remember to put lread_from_other_prec=F.

If continuation is done in a new run directory, ﬁrst execute start.csh there and then copy

the ﬁles var.dat (and if present global.dat) from the old to the new directory, using pc -

copyvar.

F.2 Remeshing (regridding)

[This should be written up in a better way and put somewhere else. But currently,

remeshing is only available for the Pencil developers anyway.]

Suppose you have a directory run 64 with a 643run (running on N0=

=2×1CPUs)

that you want to continue from ‘VAR1’ at 1283(on

=4×4CPUs).

1. The remeshing code is part of the PENCIL CODE repository.

2. Create another run directory with current ‘VAR1’ as ‘var.dat’ (remesh.csh so far

only works with ‘var.dat’):

unix> cd run_64

run_64> pc_newrun ../tmp_64

new tmp_64

run_64> mkdir -p ../tmp_64/data

(cd ../tmp_64/; crtmp)

run_64> (cd ../tmp_64/data ; mkproc-tree N0)

run_64> restart-new-dir-VAR ../tmp_64 1

3. Create the new run directory (linking the executables with -s):

run_64> cd ../tmp_64

tmp_64> pc_newrun -s ../run_128

new run_128

tmp_64> vi ../run_128/src/cparam.local

# set nxgrid=128, ncpus=16, nprocy=4

tmp_64> (cd ../run_128; crtmp; pc_setupsrc; make)

4. Setup and do remeshing

tmp_64> setup-remesh

tmp_64> vi remesh/common.local

# set muly=2, mulz=4, remesh par=2

tmp_64> (cd remesh; make)

tmp_64> vi remesh.in

# Replace line by ../run 128

tmp_64> remesh.csh

# Answer ‘yes’

F.3 Restarting from a run with less physics 147

F.3 Restarting from a run with less physics

First, prepare a new run directory with the new physics included. By new physics, we

mean that the new run wants to read in more ﬁelds (e.g. magnetic ﬁelds, if the old run

didn’t have magnetic ﬁelds).

Example for test ﬁelds:

1. Prepare ‘src/cparam.local’

Add the following 2 fragments into the ‘cparam.local’ ﬁle. The ﬁrst piece comes in

the beginning and the second in the end of the ﬁle.

!** AUTOMATIC CPARAM.INC GENERATION ****************************************

! Declare (for generation of cparam.inc) the number of f array

! variables and auxiliary variables added by this module

! Use MVAR to reserve the appropriate workspace for testfield_z.f90

! The MAUX number must be equally big and is used for uxb in the f-array.

! At the end of this file, njtest must be set such that 3*njtest=MVAR.

! MVAR CONTRIBUTION 12

! MAUX CONTRIBUTION 12

!***************************************************************************

! note that MVAR=MAUX=3*njtest must be obeyed

integer, parameter :: njtest=4

2. Prepare ‘src/Makefile.local’

Add the line TESTFIELD=testfield_z to the ﬁle. Finally, compile the code.

3. Prepare restart data

Go into data directory of the new run and prepare the directory tree using, e.g., the

command pc_mkproctree 16. [In principle this could be automatized, but it isn’t

yet.]

Next, go into old run directory and say restart-new-dir ../32c, if ‘../32c’ is the

name of the new run directory. This procedure copies all the ﬁles from the processor

tree, plus ﬁles like ‘param.nml’, but this ﬁle may need some manual modiﬁcation (or

you could just us one from another runs with the new physics included, which is

deﬁnitely the simplest!).

4. Prepare ‘run.in’

Set lread_oldsnap_notestfield=T in

run pars

. This means (as the name says) that

one reads an old snapshot that did not have test ﬁelds in it.

Reset boundary conditions and add stuff for the newly added ﬁelds, e.g.,

bcz=’a:s’,’a’,’a:s’,’a2’,’a’,’a’,’s’,’a’,’a’,’s’,’a’,’a’,’s’,’a’,’a’,’s’

run pars

. If you don’t do this, you would effectively use periodic boundary

conditions for the response to the test ﬁeld, which is hardly correct once you set

non-periodic boundary conditions for the other variables.

148 THE PENCIL CODE

Add something like the following text fragments in the right position (after

grav -

run pars

and

magnetic run pars

, but before

shear run pars

and

viscosity run -

pars

&testfield_run_pars

!linit_aatest=T, daainit=100.

itestfield=’B11-B22’

etatest=1e-4

lsoca=F

Make sure that the data above are correct. You may want to change the values of

daainit

etatest

If you now run, and if you didn’t ﬁx the ﬁle ‘data/param.nml’ you might get some-

thing like the following error:

forrtl: severe (24): end-of-file during read, unit 1, file /wkspace/brandenb/pencil-code/axel/Poiseuille/2d/32c/data/pa

The reason for this is that it reads the old boundary data, but the correspond-

ing array is too short. This includes stuff like

FBCX1

FBCX2 2

, but it is still

not enough. Therefore it is easiest to use the ‘data/param.nml’ ﬁle from another

run. You may well just use one from a single processor run with a different mesh.

But remember to ﬁx the ‘start.in’ ﬁle by correcting the boundary conditions and

adding things like

&testfield_init_pars

luxb_as_aux=T

5. Prepare ‘print.in’, ‘xyaver.in’, and other obvious ﬁles such as ‘video.in’.

6. Once it works and is running, you must say explicitly

&run_pars

...

lread_oldsnap_notestfield=F

because otherwise you won’t read in your precious test ﬁeld data next time you

restart the code! (If you instead just remove this line, it will remember lread_-

oldsnap_notestfield=T from the previous run, which is of course wrong!)

Comments: For large magnetic Reynolds numbers the solutions to the test-ﬁeld equa-

tions can show a linear instability, which can introduce large ﬂuctuations. In that case

it is best to reset the dependent test-ﬁeld variable to zero in regular intervals. This is

done by setting linit aatest=T. Note that daainit=100 sets the reset interval to 100.

F.4 Restarting with particles from a run without them

If you want to restart from a run without particles to a run with them, you need to

(1) Compile a run with particles,

RunWithParticles$ pc_build

F.4 Restarting with particles from a run without them 149

(2) Copy a VARN or var.dat into this new run directory. Say the old run is at the directory

OldRun and you want to copy the var.dat of that run and restart with particles. You do

RunWithParticles$ pc_copyvar v v ../OldRun . -e

(3) In the start.in init pars of the new run, add the lines

lread_oldsnap = T

ireset_tstart = 0

(4) Remove all calls to initial conditions (make all initlnrho, inituu, initss, initaa, etc

‘nothing’), and

5) Run pc_start.

The variable lread_oldsnap makes the code on start time read from the f-array of the

snapshot, instead of the default, which is to initialize it with zeros. The necessity in step

(4) to remove all calls to initial conditions is because otherwise the code would rewrite

the content of the f-array with these initial conditions, or add them on top of the existing

values of the snapshot.

The variable ireset_tstart when set to zero makes it read the timestamp of the old

snapshot and restart from that time. The default is 2, which sets the timestamp back to

zero.

150 THE PENCIL CODE

G Runs and reference data

For reference purposes we document here some results obtained with various samples

of the code.

G.1 Shock tests

G.1.1 Sod shock tube problem

Table 15: Combinations of ρ,p, and s/cpthat are relevant for the Sod shock tube problem with constant

temperature and different pressure ratios on the left and right hand sides of the shock.

ρ p s

1.0 1.0 0.3065

0.1 0.1 1.2275

0.01 0.01 2.1486

G.1.2 Temperature jump

Table 16: Combinations of c2

s,p, and s/cpthat are relevant for the temperature shock problem with

constant density, ρ= 1, and different temperature ratios on the left and right hand sides of the shock.

1.0 0.0

0.1 −2.3

0.01 −4.6

10−4−9.2

G.2 Random forcing function

A solenoidal random forcing function fcan be invoked by putting iforce=’helical’ in

the

forcing run pars

namelist. This produces the forcing function fof the form

f(x, t) = Re{Nfk(t)exp[ik(t)·x+iφ(t)]},(222)

where k(t) = (kx, ky, kz)is a time dependent wave vector, x= (x, y, z)is position, and

φ(t)with |φ|< π is a random phase. On dimensional grounds the normalization factor

is chosen to be N=f0cs(kcs/δt)1/2, where f0is a nondimensional factor, k=|k|, and δt

is the length of the timestep. The δt−1/2dependence ensures that the forcing, which is

delta-correlated in time, is properly normalized such that the correlator of the forcing

function is independent of the length of the time step, δt. We focus on the case where

|k|is around 5, and select at each timestep randomly one of the 350 possible vectors in

4.5<|k|<5.5. We force the system with eigenfunctions of the curl operator,

fk=ik×(k×e)−σ|k|(k×e)

√1 + σ2k2q1−(k·e)2/k2,(223)

G.3 Three-layered convection model 151

where eis an arbitrary unit vector needed in order to generate a vector k×ethat is

perpendicular to k. Note that |fk|2= 1 and, for σ= 1,ik×fk=|k|fk, so the helicity

density of this forcing function satisﬁes

f·∇×f=|k|f2>0 (for σ= 1) (224)

at each point in space. We note that since the forcing function is like a delta-function in

k-space, this means that all points of fare correlated at any instant in time, but are dif-

ferent at the next timestep. Thus, the forcing function is delta-correlated in time (but the

velocity is not). This is the forcing function used in Brandenburg (2001), Brandenburg

& Dobler (2001), and other papers in that series.

For σ= 0, the forcing function is completely nonhelical and reduces to the simpler form

fk= (k×e)/qk2−(k·e)2.(225)

For 0<|σ|<1, the forcing function has fractional helicity, where σ≈ hω·ui/(kfhu2i);

see Sect. 4.5 of Ref. [9]. In the code and the

forcing run pars

namelist, σis called

relhel

In the code, the possible wavevectors are pre-calculated and stored in ‘k.dat’, which

is being read in the beginning the code runs. To change the wavevectors (e.g.

the typical value of kf, you need to change the ﬁle. In the directory ‘$PENCIL_-

HOME/samples/helical-MHDturb/K_VECTORS/’ there are several such ﬁles prepared:

k10.dat k1.dat k2.dat k3.dat k5.dat

k15.dat k27.dat k30.dat k4.dat k8.dat

and more can be prepared in IDL with the procedure ‘$PENCIL_-

HOME/samples/helical-MHDturb/idl/generate_kvectors.pro’ There is also more help in

the ‘README’ ﬁle in ‘helical-MHDturb’.

G.3 Three-layered convection model

ln ρ

−1 0 1 2 3

−0.5

0.0

0.5

1.0

1.5

−0.15−0.10−0.050.000.05

−0.5

0.0

0.5

1.0

1.5

Entropy s

−0.6−0.4−0.20.0 0.2 0.4

−0.5

0.0

0.5

1.0

1.5

Temperature T

0.5 1.0 1.5 2.0

−0.5

0.0

0.5

1.0

1.5

Figure 21: Like in Fig. 2, but at time t= 50.

In Sect. 3 we have shown the early stages of the convection model located in

‘samples/conv-slab’. To arrive at fully developed convection, you will need to run the

152 THE PENCIL CODE

0 10 20 30 40 50

0.001

0.010

0.100

1.000

umax

urms

Figure 22: Time evolution of rms and maximum velocity for the model ‘samples/conv-slab’. Similar plots

can be produced by running the IDL script ‘ts.pro’.

code for many more time steps. Figure 21 shows the vertical proﬁles of four basic quan-

tities at time t= 50. Figure 22 shows the time evolution of rms and maximum velocity

for the model for 0< t < 50.

Figures 23 and 24 show vertical and horizontal sections for time t= 50.

u at z=−0.292903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

u at z=−0.292903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

u at z=0.352258

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

u at z=0.352258

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

u at z=0.932903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

u at z=0.932903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

s and ρ at z=−0.292903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

s and ρ at z=0.352258

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

s and ρ at z=0.932903

−0.4−0.2 0.0 0.2 0.4

−0.4

−0.2

0.0

0.2

0.4

Figure 23: Horizontal sections for t= 50. Top: velocity ﬁeld. Bottom: entropy (color coded) and density

(isocontours). Plots of this type can be produced by running the IDL script ‘hsections.pro’)

G.4 Magnetic helicity in the shearing sheet

To test magnetic helicity evolution in the shearing shear, we can choose as initial

condition initaa=’Beltrami-y’ with amplaa=1. in magnetic_init_pars together with

Sshear=-1. in shear_run_pars.

G.4 Magnetic helicity in the shearing sheet 153

u at y=−0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

u at y=−0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

u at y=0.0156250

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

u at y=0.0156250

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

u at y=0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

u at y=0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

s and ρ at y=−0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

s and ρ at y=0.0156250

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

s and ρ at y=0.296875

−0.4 −0.2 0.0 0.2 0.4

−0.5

0.0

0.5

1.0

Figure 24: Vertical section y= 0.516 at t= 50. Top: velocity ﬁeld. Bottom: entropy (color coded) and

density (isocontours). Plots of this type can be produced by running the IDL scripts ‘vsections.pro’) or

‘vsections2.pro’).

Thus, in ‘src/Makefile.local’ we just use

MAGNETIC=magnetic

HYDRO=nohydro

EOS=noeos

DENSITY=nodensity

SHEAR=shear

VISCOSITY=noviscosity

and put

&init_pars

cvsid=’$Id$’,

&magnetic_init_pars

initaa=’Beltrami-y’, amplaa=1.

&shear_init_pars

154 THE PENCIL CODE

Figure 25: Wind-up of the magnetic ﬁeld leads to a linear increase in the rms magnetic ﬁeld strength

until Ohmic diffusion begins to become important (top panel). During this time the magnetic helicity is

conserved. With Ohmic diffusion, the decay of hA·Biis well described by integrating −2ηhJ·Bi(indicated

by “from rhs” in the second panel).

in ‘start.in’ and, for example,

&run_pars

cvsid=’$Id$’

nt=150000, it1=10, cdt=0.9, isave=50, itorder=3

dsnap=100. dvid=5., ialive=1

&magnetic_run_pars

eta=0.

&shear_run_pars

Sshear=-1.

in ‘run.in’. The output includes, among other things

arms(f10.7)

G.4 Magnetic helicity in the shearing sheet 155

brms(f12.7)

jrms(f14.7)

abm(f14.11)

jbm(f14.7)

The result is shown in Figure 25, where we show the wind-up of the magnetic ﬁeld,

which leads to a linear increase in the rms magnetic ﬁeld strength until Ohmic diffu-

sion begins to become important (top panel). During this time the magnetic helicity is

conserved. With Ohmic diffusion, the decay of hA·Biis well described by integrating

−2ηhJ·Bi(indicated by “from rhs” in the second panel).

156 THE PENCIL CODE

H Numerical methods

H.1 Sixth-order spatial derivatives

Spectral methods are commonly used in almost all studies of ordinary (usually incom-

pressible) turbulence. The use of this method is justiﬁed mainly by the high numerical

accuracy of spectral schemes. Alternatively, one may use high order ﬁnite differences

that are faster to compute and that can possess almost spectral accuracy. Nordlund &

Stein [30] and Brandenburg et al. [14] use high order ﬁnite difference methods, for ex-

ample fourth and sixth order compact schemes [26].18

The sixth order ﬁrst and second derivative schemes are given by

f′

i= (−fi−3+ 9fi−2−45fi−1+ 45fi+1 −9fi+2 +fi+3)/(60δx),(226)

f′′

i= (2fi−3−27fi−2+ 270fi−1−490fi+ 270fi+1 −27fi+2 + 2fi+3)/(180δx2),(227)

In Fig. 26 we plot effective wavenumbers for different schemes. Apart from the different

explicit ﬁnite difference schemes given above, we also consider a compact scheme of 6th

order, which can be written in the form

3f′

i−1+f′

i+1

3f′

i+1 = (fi−2−28fi−1+ 28fi+1 −fi+2)/(36δx),(228)

for the ﬁrst derivative, and

11 f′′

i−1+f′′

i+2

11 f′′

i+1 = (3fi−2+ 48fi−1−102fi+ 48fi+1 + 3fi+2)/(44δx2).(229)

for the second derivative. As we have already mentioned in the introduction, this scheme

involves obviously solving tridiagonal matrix equations and is therefore effectively non-

local.

In the second panel of Fig. 26 we have plotted effective wavenumbers for second deriva-

tives, which were calculated as

(cos kx)′′

num =−k2

eﬀ cos kx. (230)

Of particular interest is the behavior of the second derivative at the Nyquist frequency,

because that is relevant for damping zig-zag modes. For a second-order ﬁnite difference

scheme k2

eﬀ is only 4, which is less than half the theoretical value of π2= 9.87. For

fourth, sixth, and tenth order schemes this value is respectively 5.33, 6.04, 6.83. The

last value is almost the same as for the 6th order compact scheme, which is 6.86. Signif-

icantly stronger damping at the Nyquist frequency can be obtained by using hypervis-

cosity, which Nordlund & Galsgaard (1995) treat as a quenching factor that diminishes

the value of the second derivative for wavenumbers that are small compared with the

Nyquist frequency. Accurate high order second derivatives (with no quenching factors)

are important when calculating the current Jin the Lorentz force J×Bfrom a vector

potential Ausing −µ0J=∇2A−∇∇·A. This will be important in the MHD calculations

presented below.

18The fourth order compact scheme is really identical to calculating derivatives from a cubic spline,

as was done in Ref. [30]. In the book by Collatz [15] the compact methods are also referred to as Her-

mitian methods or as Mehrstellen-Verfahren, because the derivative in one point is calculated using the

derivatives in neighboring points.

H.2 Upwind derivatives to avoid ‘wiggles’ 157

Figure 26: Effective wave numbers for ﬁrst and second derivatives using different schemes. Note that

for the second derivatives the sixth order compact scheme is almost equivalent to the tenth order explicit

scheme. For the ﬁrst derivative the sixth order compact scheme is still superior to the tenth order explicit

scheme.

H.2 Upwind derivatives to avoid ‘wiggles’

High-order centered-difference convection simulations often show “wiggles” (Nyquist

zigzag pattern) in ln ρ, which are apparently caused by a velocity proﬁle where the veloc-

ity approaches zero on the boundary or inside the box.19 This causes the density proﬁle

to be squeezed into a boundary layer where eventually numerical resolution is insufﬁ-

cient and, for centered differences, a spurious Nyquist signal is generated that almost

instantaneously propagates into much of the whole box.

Even if the stagnation point is on the boundary (and enforced by the boundary con-

ditions), this behavior is hardly inﬂuenced by the boundary conditions on ln ρat all.

A solution, however, is to apply upwinded derivative operators. The simplest upwind

derivative is a ﬁnite-difference derivative operator where the point furthest downwind

is excluded from the stencil. For u > 0, that means that instead of

f′

0=−f−3+ 9f−2−45f−1+ 45f1−9f2+f3

60 δx −δx6f(7)

140 =D(cent,6) +Oδx6,(231)

one takes

f′

0=−2f−3+ 15f−2−60f−1+ 20f0+ 30f1−3f2

60 δx +δx5f(6)

60 =D(up,5) +Oδx5.(232)

A fourth-order upwind scheme (excluding two downwind points) would be

f′

0=−f−3+ 6f−2−18f−1+ 10f0+ 3f1

12 δx −δx4f(5)

20 =D(up,4) +Oδx4.(233)

19A simple one-dimensional test proﬁle would be u(x) = 1 −x2on x∈[−1,1], which will accumulate

more and more mass near the right boundary x= 1.

In two- or three-dimensional settings, the presence of stagnation points of X-type leads to the same

conﬁguration, this time with the possibility of a steady state (i.e. without accumulation of mass). Such

stagnation points occur e.g. at the top of an upwelling, or at the bottom of a downdraft in convection

simulations, where locally uz∝zX−z.

158 THE PENCIL CODE

The effect of upwinding is mostly to stop the Nyquist perturbations from spreading away

from the boundary or stagnation point. With the fourth-order formula they actually

hardly ever develop.

The difference between central and ﬁfth-order upwind derivative is

[D(up,5) −D(cent,6)]f0=−f−3+ 6f−2−15f−1+ 20f0−15f1+ 6f2−f3

60 δx =−δx5

60 f(6)

0.(234)

In other words, 5th-order upwinding can be represented for any sign of uas hyperdiffu-

sion (Dobler et al. 2006):

−uf′

(up,5th) =−uf′

(centr,6th) +|u|δx5

60 f(6) .(235)

The advantage over adopting constant hyperdiffusion is that in the upwinding scheme

hyperdiffusion is only applied where it is needed (i.e. where advection is happening,

hence the factor |u|).

The form (235) also suggests an easy way to get ‘stronger’ upwinding: Rather than ex-

cluding more points in the downwind direction, we can simply treat the weight of the

hyperdiffusion term as a free parameter α:

−uf′

(up,5th,α)=−uf′

(centr,6th) +α|u|δx5f(6) .(236)

If αis large, this may affect the time step, but for α= 1/60, the stability requirement for

the hyperdiffusive term should always be weaker than the advective Courant criterion.

H.3 The bidiagonal scheme for cross-derivatives

The old default scheme used for cross-derivatives of type ∂2/(∂x∂y)used to read as fol-

lows:

df=fac*( &

270.*( f(l1+1:l2+1,m+1,n,k)-f(l1-1:l2-1,m+1,n,k) &

+f(l1-1:l2-1,m-1,n,k)-f(l1+1:l2+1,m-1,n,k)) &

- 27.*( f(l1+2:l2+2,m+2,n,k)-f(l1-2:l2-2,m+2,n,k) &

+f(l1-2:l2-2,m-2,n,k)-f(l1+2:l2+2,m-2,n,k)) &

+ 2.*( f(l1+3:l2+3,m+3,n,k)-f(l1-3:l2-3,m+3,n,k) &

+f(l1-3:l2-3,m-3,n,k)-f(l1+3:l2+3,m-3,n,k)) &

)

and is “visualized” in the left part of Fig. 27. It is way more efﬁcient than the straight-

forward approach of ﬁrst taking the xand the yderivative consecutively. (shown in the

right part of Fig. 27).

Off-diagonal terms enter not only the diffusion terms through ∇∇ ·uand ∇∇ ·Aterms,

but also through the J=∇×∇×Aoperator. The general formula is Ji=Aj,ij −Ai,jj ,

so in 2-D in the xy-plane we have

Jx=Ax,xx +Ay,xy −Ax,xx −Ax,yy =Ay,xy −Ax,yy ,(237)

Jy=Ax,yx +Ay,yy −Ay,xx −Ay,yy =Ax,yx −Ay,xx (238)

Figure 28 shows how the two schemes perform for the propagation of Alfv´

en waves,

H.4 The 2N-scheme for time-stepping 159

-2 0 0 0 0 0 +2

0 +27 0 0 0 -27 0

0 0 -270 0 +270 0 0

0 0 0 0 0 0 0

0 0 +270 0 -270 0 0

0 -27 0 0 0 +27 0

+2 0 0 0 0 0 -2

9 -27 135 0 -135 27 -9

-27 81 -405 0 405 -81 27

135 -405 2025 0 -2025 405 -135

0 0 0 0 0 0 0

-135 405 -2025 0 2025 -405 135

27 -81 405 0 -405 81 -27

-9 27 -135 0 135 -27 9

Figure 27: Weights of bidiagonal scheme (left) and consecutive scheme (right) for mixed derivatives

∂2/∂x∂y. The numbers shown need to be divided by 720 δx δy for the bidiagonal and by 3600 δx δy for

the consecutive scheme.

Figure 28: Alfv´

en wave for B0= (1,2,0) and k= (1,2,0) after t= 2π. The wave travels in the direction of

k. Red symbols are for the bidiagonal scheme, black symbols show results obtained using the consecutive

scheme. Already for 162mesh points there are no clear differences. For 82mesh points both schemes are

equally imprecise regarding the phase error, but the amplitude error is still quite small (but this is mainly

a property of the time stepping scheme).

˙uz=JxB0y−JyB0x,(239)

Ax=−uzB0y,(240)

Ay= +uzB0x.(241)

The initial condition (as implemented in subroutine alfven_xy) is

uz∼cos(kxx+kyy−ωt),(242)

Ax∼+B0ysin(kxx+kyy−ωt)/ω , (243)

Ay∼ −B0xsin(kxx+kyy−ωt)/ω , (244)

where ω=k·B0. The ﬁgure shows that there is no clear advantage of either scheme, so

the code uses the more efﬁcient bidiagonal one.

H.4 The 2N-scheme for time-stepping

For time stepping, higher-order schemes are necessary in order to reduce the amplitude

and phase errors of the scheme and, to some extent, to allow longer time steps. Usually

160 THE PENCIL CODE

such schemes require large amounts of memory. However, we here use the memory-

effective 2N-schemes that require only two sets of variables to be held in memory. Such

schemes work for arbitrarily high order, although not all Runge-Kutta schemes can be

written as 2N-schemes [33, 32]. Consider the ordinary differential equation (ODE)

˙u=F(u, t),(245)

which can also be used as a prototype for a system of ODEs to be solved, like the ones

obtained by spatial discretization of PDEs. The 2N-schemes construct an approximation

to the solution

u(n)≡u(tn)(246)

according to the iterative procedure

wi=αiwi−1+δt F (ui−1, ti−1),(247)

ui=ui−1+βiwi.(248)

For a three-step (RK3-2N) scheme we have i= 1, ..., 3. In order to advance the variable

ufrom u(n)at time t(n)to u(n+1) at time t(n+1) =t(n)+δt we set in Eq. (248)

u0=u(n)and, after the last step, u(n+1) =u3,(249)

with u1and u2being intermediate steps. In order to be able to calculate the ﬁrst step,

i= 1, for which no wi−1≡w0exists, we have to require α1= 0. Thus, we are left with 5

unknowns, α2,α3,β1,β2, and β3. Three conditions follow from the fact that the scheme be

third order for linear equations, so we have to have two more conditions. One possibility

is to choose the fractional times at which the right hand side is evaluated, for example

(0,1/3,2/3) or even (0,1/2,1). Yet another possibility is to require that inhomogeneous

equations of the form ˙u=tnwith n= 1 and 2 are solved exactly. The corresponding

coefﬁcients are listed in Table 17 and compared with those given by Williamson [33]. In

practice all of them are about equally good when it comes to real applications, although

we found the ﬁrst one in Table 17 (‘symmetric’) marginally better in some simple test

problems where an analytic solution was known. In Ref. [5] the accuracy of some non-

linear equations is tested.

Table 17: Coefﬁcients for different 2N-type third-order Runge-Kutta schemes. The coefﬁcients ci(which

are determined by the αi,βi) give the time for each substep, ti=t0+ciδt

scheme c1c2c3α2α3β1β2β3

symmetric 0 1/3 2/3−2/3−1 1/3 1 1/2

[predictor/corrector] 0 1/2 1 −1/4−4/3 1/2 2/3 1/2

inhomogeneous 0 15/32 4/9−17/32 −32/27 1/4 8/9 3/4

Williamson (1980) 0 4/9 15/32 −5/9−153/128 1/3 15/16 8/15

H.5 Diffusive error from the time-stepping

In many cases we use centered ﬁrst derivatives for the advection operator, so the result-

ing discretization errors are only of dispersive nature (proportional to odd derivatives). A

diffusive error can be obtained from the discretization error of the time-stepping scheme.

For the RK3-2N scheme we have

df

dtnth order

=df

dtexact

+anδtndn+1f

dtn+1 +..., (250)

H.6 Ionization 161

where an= 1/(n+ 1)! = 0.5. In particular, for n= 1 we have a1= 1/2 = 0.2and for

n= 3 we have a3= 1/24 ≈0.04. The advection operator leads to a diffusive error equal

to a1δt(u·∇)2for n= 1 and a hyperdiffusive error equal to a3δt3(u·∇)4for n= 3.

Substituting δt =cCFLδx/|u|, where cCFL is Courant-Friedrich-Lewy constant, we have a

diffusive error ν∇2with negative ν=−a1cCFL|u|δx for n= 1, and a hyperdiffusive error

−νhyp∇4with positive νhyp =a3c3

CFL|u|δx3for n= 3. The fact that the hyperdiffusive

error has a positive effective hyperdiffusivity is an important factor in the choice of this

scheme.

To decide whether the effective hyperdiffusivity from the diffusive error is signiﬁcant,

we can compare with the error that would occur had we used a third-order upwinding

scheme (Sect. H.2). In that case we would have an effective hyperdiffusive coefﬁcient

|u|δx/12 that is 1/(12a3c3

CFL)≈5.8times larger than that from the time stepping scheme.

In this sense, the hyperdiffusive error can be regarded as small.

Since the hyperdiffusive error is proportional to −∇4, we cannot directly compare with

the physical diffusion which is proportional to ∇2. Therefore we deﬁne an effective vis-

cosity as νeﬀ =νhypk2

Ny with kNy =π/δx being the Nyquist wavenumber of the mesh

of the domain covered by Nmesh points. We deﬁne Reynolds number based on the

Nyquist wavenumber as ReNy =|u|/νeﬀ kNy, and ﬁnd Re =−24/(πcCFL)3≈2.3for our

favorite choice cCFL = 0.7. Thus, at the scale of the mesh, the effective Reynolds number

is comparable to the value often obtained in simulations. However, in turbulence sim-

ulations the viscous cutoff wavenumber is usually 5–10 times smaller than kNy, so the

relevant Reynolds number at the viscous scale is then another 2–3 orders of magnitude

larger and does therefore not impose a constraint in view of the physical viscosity that

is applied in such calculations.

H.6 Ionization

The speciﬁc entropy of each particle species (neutral hydrogen, electrons, protons and

neutral helium) may be written as

=xi ln "1

xtot

ρi

ρT

T03/2#+5

2!,(251)

where

xH= 1 −y , xe=xp=y , xtot = 1 + y+xHe (252)

s0=kB

µmH

, T0=χH

,(253)

and

ρi=µmHmiχH

2π~23/2.(254)

The speciﬁc entropy of mixing is

smix

=−X

xiln xi

xtot

.(255)

162 THE PENCIL CODE

Summing up everything, we get the total speciﬁc entropy

+smix

xi ln "1

ρi

ρT

T03/2#+5

2!(256)

xiln ρi

+xtot ln "1

ρT

T03/2#+5

2!.(257)

Solving for Tgives

2ln T

=s/s0+Pixiln xi/ρi

xtot

+ ln ρ−5

2.(258)

Using this expression and the constants deﬁned above, we may obtain the ionization

fraction yfor given ln ρand sby ﬁnding the root of

F= ln "ρe

ρT

T03/21−y

y2#−T0

T.(259)

The derivative with respect to yfor Newton-Raphson is

∂F

∂y =3

2+T0

T∂ln T/T0

∂y −1

1−y−2

y,(260)

where

∂ln T/T0

∂y =

3(ln ρH/ρp−F−T0/T )−1

1 + y+xHe

.(261)

In order to compute the pressure gradient in the momentum equation, the derivative of

ywith respect to ln ρand sneeds to be known:

∂ln P

∂ln ρ=1

1 + y+xHe

∂y

∂ln ρ+∂ln T

∂y

∂ln ρ+ 1,(262)

∂ln P

∂s =1

1 + y+xHe

∂y

∂s +∂ln T

∂y

∂s .(263)

Since F= 0 for all desired solutions (y, ln ρ, s)we also have

dF =∂F

∂ln ρd ln ρ+∂F

∂s ds+∂F

∂y dy= 0 ,(264)

and thus ∂y

∂ln ρ=dy

d ln ρds=0

=−∂F/∂ ln ρ

∂F/∂y (265)

and ∂y

∂s =dy

dsd ln ρ=0

=−∂F/∂s

∂F/∂y .(266)

H.7 Radiative transfer

H.7.1 Solving the radiative transfer equation

A formal solution of Eq. (81) is given by

I(τ) = I(τ0)e−(τ−τ0)+

τ0

e−(τ−τ′)S(τ′)dτ′.(267)

H.7 Radiative transfer 163

Using a generalization of the trapezoidal rule,

τ0

e−(τ−τ′)f(τ′)dτ′≈

τ0

e−(τ−τ′)f(τ0) + f(τ)−f(τ0)

τ−τ0

(τ′−τ0)dτ′(268)

=1−e−(τ−τ0)f(τ)−1−e−(τ−τ0)(1 + τ−τ0)

τ−τ0

[f(τ)−f(τ0)] ,(269)

which is exact for linear functions S(τ), we discretize this as

Ik+1 =Ike−δτ + (1−e−δτ )Sk+1 −1−e−δτ (1 + δτ)

δτ (Sk+1 −Sk),(270)

=Ike−δτ + (1−e−δτ )Sk+e−δτ −1 + δτ

δτ (Sk+1 −Sk).(271)

Here the simplest way to calculate δτ is

δτ =χk+χk+1

2δx ;(272)

more accurate alternatives are

δτ =√χkχk+1 δx (273)

δτ =χk+1 −χk

ln χk+1

ln χk

δx (274)

H.7.2 Angular integration

Table 18: Sums √4πY m

l(θi, φi)for special sets of directions. For all degrees and orders up to l= 8 not

mentioned in this table, the sums are 0. The label ‘Non-h. f-d.’ stands for ‘non-horizontal face-diagonals’,

i.e. the eight face diagonals that are not in the horizontal plane.

Directions Y0

0Y0

2Y0

4Y±4

4Y0

6Y±4

6Y0

8Y±4

8Y±8

Coord. 6 0 21

4√70 3

4√13 −3

8√182 99

32√17 3

32√2618 3

64√24310

Face diag. 12 0 −21

4−3

8√70 −39

16√13 39

32√182 891

256√17 27

256√2618 27

512√24310

Space diag. 8 0 −28

3−2

3√70 16

9√13 −8

9√182 11

9√17 1

27√2618 1

54√24310

Non-h. f-d. 8 2√5−39

8√70 −19

16√13 27

32√182 611

256√17 51

256√2618 3

512√24310

Coord. x,y4−2√59

3√70 −5

4√13 −3

8√182 35

32√17 3

32√2618 3

64√24310

Coord. z2 2√5 6 0 2√13 0 2√17 0 0

For angular integration over the full solid angle, we make the ansatz

4π

f(θ, φ)dω

4π=

i=1

wif(θi, φi) + RN.(275)

164 THE PENCIL CODE

Table 18 shows the sums √4πY m

l(θi, φi)over special sets of directions (θi, φi). Using these

numbers and requiring that angular integration is exact for l≤lmax, we ﬁnd the follow-

ing weights wifor different sets of directions (see also [1], §25.4.65).20

Cooling times have been determined numerically in [3]. Comparing with analytic ex-

pressions obtained in the Eddington approximation, the proposed suitable switches in

1-D and 2-D problems.

1. Axes

Coordinate axes: 1/6

lmax = 3

2. Face diagonals

Face diagonals: 1/12

lmax = 3

3. Space diagonals

Space diagonals: 1/8

lmax = 3

4. Axes + face diagonals

Coordinate axes: 1/30

Face diagonals: 1/15

lmax = 5

5. Axes + space diagonals

Coordinate axes: 1/15

Space diagonals: 3/40

lmax = 5

6. Face + space diagonals

Face diagonals: 2/15

Space diagonals: -3/40

lmax = 5

7. Axes, face + space diagonals

Coordinate axes: 1/21

Face diagonals: 4/105

Space diagonals: 9/280

lmax = 7

8. Axes, non-horizontal face diagonals

Coordinate axes x,y: 1/10

Coordinate axes z: 1/30

Non-hor. face diagonals: 1/15

lmax = 3

9. Axes, non-horizontal face diagonals, space diagonals

Coordinate axes x,y: 12/215

Coordinate axes z: 10/129

Non-hor. face diagonals: -14/645

Space diagonals: 171/1720

lmax = 5

I. Curvilinear coordinates 165

I Curvilinear coordinates

The use and implementation of non-cartesian coordinate systems is brieﬂy explained in

Section 5.25. All differential operators look like their cartesian counterparts, except that

all derivatives are now replaced by covariant derivatives. The relevant reference for the

PENCIL CODE is [28]; see their Appendix B. Here some details.

I.1 Covariant derivatives

Aˆα;ˆ

β=Aˆα, ˆ

β−Γˆσ

ˆαˆ

βAˆσ,(276)

Aˆαˆ

β;ˆγ=Aˆαˆ

β,ˆγ−ΓˆσˆαˆγAˆσˆ

β−Γˆσˆ

βˆγAˆαˆσ.(277)

Second derivative tensor

Aˆα;ˆ

βˆγ=Aˆα;ˆ

β,ˆγ−ΓˆσˆαˆγAˆσ;ˆ

β−Γˆσˆ

βˆγAˆα;ˆσ

=Aˆα, ˆ

βˆγ−Γˆσ

ˆαˆ

βAˆσ,ˆγ−Γˆσ

ˆαˆ

β,ˆγAˆσ−ΓˆσˆαˆγAˆσ, ˆ

β+ ΓˆσˆαˆγΓˆν

ˆσˆ

βAˆν−Γˆσˆ

βˆγAˆα,ˆσ+ Γˆσˆ

βˆγΓˆνˆαˆσAˆν.

Elements of the ﬁrst derivative tensor

Aˆr;ˆr=Aˆr,ˆr, Aˆ

θ;ˆ

θ=Aˆ

θ,ˆ

θ+r−1Aˆr, Aˆ

φ;ˆ

φ=Aˆ

φ, ˆ

φ+r−1Aˆr+r−1cotθ Aˆ

θ.(278)

Aˆ

φ;ˆ

θ=Aˆ

φ,ˆ

θAˆ

θ;ˆ

φ=Aˆ

θ, ˆ

φ−r−1cotθ Aˆ

Aˆr;ˆ

φ=Aˆr, ˆ

φ−r−1Aˆ

φAˆ

φ;ˆr=Aˆ

φ,ˆr

Aˆ

θ;ˆr=Aˆ

θ,ˆrAˆr;ˆ

θ=Aˆr,ˆ

θ−r−1Aˆ

(279)

I.2 Differential operators

All differential operators look like their cartesian counterparts, except that all deriva-

tives are now replaced by covariant derivatives.

I.2.1 Gradient

For the gradient operator the covariant and partial derivatives are the same, i.e.

∇Ψ = Ψ;ˆα= Ψ,ˆα=



∂ˆrΨ

∂ˆ

θΨ

∂ˆ

φΨ

(280)

where

∂ˆr=∂r(281)

∂ˆ

θ=r−1∂θ(282)

∂ˆ

φ=̟−1∂φ(283)

and ̟=rsin θis the cylindrical radius. Thus,

∇Ψ=(∇Ψ)(0) ,(284)

166 THE PENCIL CODE

where the superscript (0) indicated the straightforward calculation in the non-

coordinate basis. The coordinate and non-coordinate bases are related to each other

via

(∇Ψ)0≡



Ψ,ˆr

Ψ,ˆ







1 0 0

0r−10

0 0 ̟−1

(∇Ψ)(coord) .(285)

Here, the result in the coordinate basis is just what one would get by computing as if

one had cartesian coordinates. In the PENCIL CODE the output or the subroutine der is

now in this non-coordinate basis.

I.2.2 Divergence

For the divergence operator we have a ‘correction term’, i.e.

∇·A=Aˆα; ˆα(286)

=Aˆα,ˆα+ Γˆαˆ

βˆαAˆ

β,(287)

where the only non-vanishing contributions to the last term are

Γˆαˆ

βˆαAˆ

β= Γˆ

ˆrˆ

θAˆr+ Γˆ

ˆrˆ

φAˆr+ Γˆ

φˆ

θˆ

φAˆ

θ(288)

= 2r−1Aˆr+r−1cotθ Aˆ

θ.(289)

Thus,

∇·A= (∇·A)(0) +M(div)

ˆαAˆα,(290)

where

M(div)

ˆα=



2r−1

r−1cotθ

0

(291)

represents the correction term.

Alternatively:

Aˆα; ˆα=Aˆα, ˆα−ΓˆσˆαˆαAˆσ(292)

=Aˆα, ˆα+ 2r−1Aˆr+r−1cotθ Aˆ

θ.(293)

I.2.3 Curl

The curl operator is given by

(∇×B)ˆα=ǫˆαˆ

βˆγBˆγ, ˆ

β.(294)

∇×A=



Aˆ

φ;ˆ

θ−Aˆ

θ;ˆ

Aˆr;ˆ

φ−Aˆ

φ;ˆr

Aˆ

θ;ˆr−Aˆr;ˆ



(295)

∇×A=





Aˆ

φ,ˆ

θ−Aˆ

θ, ˆ

φ+ Γˆ

φˆ

θˆ

φAˆ

Aˆr, ˆ

φ−Aˆ

φ,ˆr−Γˆ

φˆrˆ

φAˆ

Aˆ

θ,ˆr−Aˆr,ˆ

θ+ Γˆ

θˆrˆ

θAˆ

θ



(296)

I.2 Differential operators 167

Thus,

∇×A= (∇×A)(0) +M(curl)

ˆαˆ

βAˆ

β,(297)

where

M(curl)

ˆαˆ

β=



0 0 r−1cotθ

0 0 −r−1

0r−10

(298)

is the correction term. In the PENCIL CODE we use the subroutine curl mn(aij,bb,aa),

which uses aij=Aˆα, ˆ

βand aa=Aˆαas input pencils and produces bb=Bˆαas output.

I.2.4 Advection operator

[The usage of roman indices here is insigniﬁcant.]

u·∇u=ω×u+1

2∇u2=−u×ω+1

2∇u2(299)

(u·∇u)i=−ǫijkǫklmujum;l+ujuj,i

= (−δilδjm +δimδjl)ujum;l+ujuj,i

=−ujuj;i+ujui;j+ujuj,i

=ujui;j+ Γkjiujuk

=ujui,j + (−Γkij + Γkji)ujuk(300)

Note that the terms with Γˆrˆ

θˆ

θ,Γˆrˆ

φˆ

φ, and Γˆ

θˆ

φˆ

φdrop out. Thus, we have

(u·∇u)ˆr=ujuˆr,j + (−Γkˆrj + Γkjˆr)ujuk

=ujuˆr,j −Γˆ

ˆrˆ

θu2

θ−Γˆ

ˆrˆ

φu2

=ujuˆr,j −r−1(u2

θ+u2

φ)(301)

(u·∇u)ˆ

θ=ujuˆ

θ,j + (−Γkˆ

θj + Γk

jˆ

θ)ujuk

=ujuˆ

θ,j −Γˆ

φˆ

θˆ

φu2

φ+ Γˆ

ˆrˆ

θuˆruˆ

=ujuˆ

θ,j −r−1cotθ u2

φ+r−1uˆruˆ

θ(302)

(u·∇u)ˆ

φ=ujuˆ

φ,j + (−Γkˆ

φj + Γk

jˆ

φ)ujuk

=ujuˆ

φ,j + Γˆ

ˆrˆ

φuˆruˆ

φ+ Γˆ

φˆ

θˆ

φuˆ

θuˆ

=ujuˆ

φ,j +r−1uˆruˆ

φ+r−1cotθ uˆ

θuˆ

φ(303)

Note that the formulation above is slightly misleading, because

Γk

jˆ

θujuk= Γˆrˆ

θˆ

θuˆ

θuˆr+ Γˆ

ˆrˆ

θuˆruˆ

θ= 0 (304)

Γk

jˆ

φujuk= Γˆrˆ

φˆ

φuˆ

φuˆr+ Γˆ

ˆrˆ

φuˆruˆ

φ+ Γˆ

θˆ

φˆ

φuˆ

θ+ Γˆ

φˆ

θˆ

φuˆ

θuˆ

φ= 0 (305)

I.2.5 Mixed advection operator

u×B=u×∇B=ujǫijkǫklmAm;l=uj(δilδjm −δimδjl)Am;l=ujAj;i−ujAi;j(306)

168 THE PENCIL CODE

I.2.6 Shear term

ujAj;i= (ujAj);i−uj;iAj= (ujAj),i −uj;iAj(307)

uj;iAj=uj,iAj−Γk

jiukAj(308)

uˆ

φ;ˆrAˆ

φ=uˆ

φ,ˆrAˆ

φ−Γk

φˆrukAˆ

φ=uˆ

φ,ˆrAˆ

φ(309)

uˆr;ˆ

φAˆr=uˆr, ˆ

φAˆr−Γˆ

ˆrˆ

φuˆ

φAˆr(310)

I.2.7 Another mixed advection operator

uˆ

βAˆα;ˆ

β=uˆ

βAˆα, ˆ

β−Γˆσ

ˆαˆ

βuˆ

βAˆσ,(311)

Write out

(u·∇A)ˆr=uˆrAˆr;ˆr+uˆ

θAˆr;ˆ

θ+uˆ

φAˆr;ˆ

φ=uˆrAˆr,ˆr,+uˆ

θAˆr,ˆ

θ−r−1uˆ

θAˆ

θ+uˆ

φAˆr, ˆ

φ−r−1uˆ

φAˆ

(u·∇A)ˆ

θ=uˆrAˆ

θ;ˆr+uˆ

θAˆ

θ;ˆ

θ+uˆ

φAˆ

θ;ˆ

φ=uˆrAˆ

θ,ˆr+uˆ

θAˆ

θ,ˆ

θ+r−1uˆ

θAˆr,+uˆ

φAˆ

θ, ˆ

φ−r−1cotθ uˆ

φAˆ

(u·∇A)ˆ

φ=uˆrAˆ

φ;ˆr+uˆ

θAˆ

φ;ˆ

θ+uˆ

φAˆ

φ;ˆ

φ=uˆrAˆ

φ,ˆr+uˆ

θAˆ

φ,ˆ

θ+uˆ

φAˆ

φ, ˆ

φ+r−1uˆ

φAˆr+r−1cotθ uˆ

φAˆ

θ.

Reorder

(u·∇A)ˆr=uˆrAˆr,ˆr+uˆ

θAˆr,ˆ

θ+uˆ

φAˆr, ˆ

φ−r−1uˆ

θAˆ

θ−r−1uˆ

φAˆ

(u·∇A)ˆ

θ=uˆrAˆ

θ,ˆr+uˆ

θAˆ

θ,ˆ

θ+uˆ

φAˆ

θ, ˆ

φ+r−1uˆ

θAˆr−r−1cotθ uˆ

φAˆ

(u·∇A)ˆ

φ=uˆrAˆ

φ,ˆr+uˆ

θAˆ

φ,ˆ

θ+uˆ

φAˆ

φ, ˆ

φ+r−1uˆ

φAˆr+r−1cotθ uˆ

φAˆ

θ.(312)

I.2.8 Strain Matrix

The strain matrix takes the form 2sˆαˆ

β=uˆα;ˆ

β+uˆ

β;ˆα. The components of the covariant

derivative tensor were given in Eqs. (278) and (279), so the ﬁnal result reads

2s≡



2uˆr,ˆruˆr,ˆ

θ+uˆ

θ,ˆr−uˆ

θ/r uˆr, ˆ

φ+uˆ

φ,ˆr−uˆ

φ/r

uˆr,ˆ

θ+uˆ

θ,ˆr−uˆ

θ/r 2uˆ

θ,ˆ

θ+ 2uˆr/r uˆ

θ, ˆ

φ+uˆ

φ,ˆ

θ−uˆ

cotθ

uˆr, ˆ

φ+uˆ

φ,ˆr−uˆ

φ/r uˆ

θ, ˆ

φ+uˆ

φ,ˆ

θ−uˆ

cotθ

r2uˆ

φ, ˆ

φ+ 2uˆr/r + 2uˆ

cotθ



(313)

The trace-less rate of strain matrix is given by

Sij =sij −1

3δij∇·u.(314)

I.2.9 Lambda effect

Qij =



0 0 ΛVΩ

0 0 ΛHΩ

ΛVΩ ΛHΩ 0 

(315)

where Ω = uˆ

φ/r sin θ. Next, compute Qij;j.

Qˆαˆ

β;ˆγ=Qˆαˆ

β,ˆγ−ΓˆσˆαˆγQˆσˆ

β−Γˆσˆ

βˆγQˆαˆσ.(316)

I.2 Differential operators 169

Qˆ

θˆr;ˆr=Qˆ

θˆr,ˆr−Γˆσˆ

θˆrQˆσˆr−ΓˆσˆrˆrQˆ

θˆσ.

= 0 (317)

Qˆ

θˆ

θ;ˆ

θ=Qˆ

θˆ

θ,ˆ

θ−Γˆσˆ

θˆ

θQˆσˆ

θ−Γˆσˆ

θˆ

θQˆ

θˆσ.

=−Γˆ

φˆ

θˆ

θQˆ

φˆ

θ−Γˆ

φˆ

θˆ

θQˆ

θˆ

φ.

= 0 (318)

Qˆ

θˆ

φ;ˆ

φ=Qˆ

θˆ

φ, ˆ

φ−Γˆσˆ

θˆ

φQˆσˆ

φ−Γˆσˆ

φˆ

φQˆ

θˆσ.

=Qˆ

θˆ

φ, ˆ

φ−Γˆ

φˆ

θˆ

φQˆ

φˆ

φ−Γˆrˆ

φˆ

φQˆ

θˆr−Γˆ

θˆ

φˆ

φQˆ

θˆ

θ.

= 0 (319)

φterms

Qˆ

φˆr;ˆr=Qˆ

φˆr,ˆr−Γˆσˆ

φˆrQˆσˆr−ΓˆσˆrˆrQˆ

φˆσ.

=Qˆ

φˆr,ˆr(320)

Qˆ

φˆ

θ;ˆ

θ=Qˆ

φˆ

θ,ˆ

θ−Γˆσˆ

φˆ

θQˆσˆ

θ−Γˆσˆ

θˆ

θQˆ

φˆσ

=Qˆ

φˆ

θ,ˆ

θ−Γˆrˆ

θˆ

θQˆ

φˆr

=Qˆ

φˆ

θ,ˆ

θ+r−1Qˆ

φˆr(321)

Qˆ

φˆ

φ;ˆ

φ=Qˆ

φˆ

φ, ˆ

φ−Γˆσˆ

φˆ

φQˆσˆ

φ−Γˆσˆ

φˆ

φQˆ

φˆσ

=−Γˆσˆ

φˆ

φQˆσˆ

φ−Γˆσˆ

φˆ

φQˆ

φˆσ

=−Γˆrˆ

φˆ

φQˆrˆ

φ−Γˆ

θˆ

φˆ

φQˆ

θˆ

φ−Γˆrˆ

φˆ

φQˆ

φˆr−Γˆ

θˆ

φˆ

φQˆ

φˆ

= +r−1Qˆrˆ

φ+ cot θ r−1Qˆ

θˆ

φ+r−1Qˆ

φˆr+ cot θ r−1Qˆ

φˆ

= +2r−1ΛVΩ + 2 cot θ r−1ΛHΩ(322)

So, the φcomponent of the divergence of the Lambda tensor is then

Qˆ

φˆσ;ˆσ=Qˆ

φˆr,ˆr+Qˆ

φˆ

θ,ˆ

θ+ 3r−1ΛVΩ + 2 cot θ r−1ΛHΩ(323)

I.2.10 Laplacian of a scalar

Let Eˆα≡(∇Ψ)ˆα=∂ˆαΨThen

∆Ψ = Eˆ

β;ˆ

β= (∂ˆ

βΨ),ˆ

β+2

rΨ,ˆr+cotθ

rΨ,ˆ

θ(324)

I.2.11 Hessian of a scalar

s;ˆα=s,ˆα(325)

s;ˆrˆr=s,ˆrˆr−Γˆσˆrˆrs,ˆσ,=s,ˆrˆr(326)

s;ˆ

θˆ

θ=s,ˆ

θˆ

θ−Γˆrˆ

θˆ

θs,ˆr,=s,ˆ

θˆ

θ+r−1s,ˆr,(327)

s;ˆ

φˆ

φ=s,ˆ

φˆ

φ−Γˆσˆ

φˆ

φs,ˆσ,=s,ˆ

φˆ

φ−Γˆrˆ

φˆ

φs,ˆr,−Γˆ

θˆ

φˆ

φs,ˆ

θ,=s,ˆ

φˆ

φ+r−1s,ˆr,+r−1cot θ s,ˆ

θ,(328)

170 THE PENCIL CODE

s;ˆrˆ

θ=s,ˆrˆ

θ−Γˆ

ˆrˆ

θs,ˆ

θ,=s,ˆrˆ

θ−r−1s,ˆ

θ,(329)

s;ˆrˆ

φ=s,ˆrˆ

φ−Γˆ

ˆrˆ

φs,ˆ

φ,=s,ˆrˆ

φ−r−1s,ˆ

φ(330)

s;ˆ

θˆr=s,ˆ

θˆr−Γˆσˆ

θˆrs,ˆσ,=s,ˆ

θˆr(331)

s;ˆ

φˆr=s,ˆ

φˆr−Γˆσˆ

φˆrs,ˆσ,=s,ˆ

φˆr(332)

s;ˆ

θˆ

φ=s,ˆ

θˆ

φ−Γˆ

φˆ

θˆ

φs,ˆ

φ,=s,ˆ

θˆ

φ−r−1cot θ s,ˆ

φ(333)

s;ˆ

φˆ

θ=s,ˆ

φˆ

θ−Γˆσˆ

φˆ

θs,ˆσ,=s,ˆ

φˆ

θ(334)

So,

s;ˆαˆ

β=s,ˆαˆ

β+



0−r−1s,ˆ

θ−r−1s,ˆ

0 +r−1s,ˆr−r−1cot θ s,ˆ

0 0 −Γˆrˆ

φˆ

φs,ˆr−Γˆ

θˆ

φˆ

φs,ˆ



(335)

I.2.12 Double curl

For the calculation of J=∇×Bwe use the same curl routine, but with different argu-

ments, bij=Bˆα, ˆ

βand bb=Bˆαas input pencils and jj=Jˆαas output, i.e. curl mn(bij,jj,bb),

so that

J=





Bˆ

φ,ˆ

θ−Bˆ

θ, ˆ

φ+ Γˆ

φˆ

θˆ

φBˆ

Bˆr, ˆ

φ−Bˆ

φ,ˆr−Γˆ

φˆrˆ

φBˆ

Bˆ

θ,ˆr−Bˆr,ˆ

θ+ Γˆ

θˆrˆ

θBˆ

θ



= (∇×B)(0) +M(curl)

ˆαˆ

βBˆ

β,(336)

where

(∇×B)(0)ˆα=ǫˆαˆ

βˆγBˆγ, ˆ

β.(337)

Expressing the components of (∇×B)(0) in terms of Aˆαwe have

Bˆ

φ,ˆ

θ= (Aˆ

θ,ˆr−Aˆr,ˆ

θ+ Γˆ

θˆrˆ

θAˆ

θ),ˆ

θBˆ

θ, ˆ

φ= (Aˆr, ˆ

φ−Aˆ

φ,ˆr−Γˆ

φˆrˆ

φAˆ

φ),ˆ

Bˆr, ˆ

φ= (Aˆ

φ,ˆ

θ−Aˆ

θ, ˆ

φ+ Γˆ

φˆ

θˆ

φAˆ

φ),ˆ

φBˆ

φ,ˆr= (Aˆ

θ,ˆr−Aˆr,ˆ

θ+ Γˆ

θˆrˆ

θAˆ

θ),ˆr

Bˆ

θ,ˆr= (Aˆr, ˆ

φ−Aˆ

φ,ˆr−Γˆ

φˆrˆ

φAˆ

φ),ˆrBˆr,ˆ

θ= (Aˆ

φ,ˆ

θ−Aˆ

θ, ˆ

φ+ Γˆ

φˆ

θˆ

φAˆ

φ),ˆ

(338)

Bˆ

φ,ˆ

θ=Aˆ

θ,ˆrˆ

θ−Aˆr,ˆ

θˆ

θ+ (Γˆ

θˆrˆ

θAˆ

θ),ˆ

θBˆ

θ, ˆ

φ=Aˆr, ˆ

φˆ

φ−Aˆ

φ,ˆrˆ

φ−(Γˆ

φˆrˆ

φAˆ

φ),ˆ

Bˆr, ˆ

φ=Aˆ

φ,ˆ

θˆ

φ−Aˆ

θ, ˆ

φˆ

φ+ (Γˆ

φˆ

θˆ

φAˆ

φ),ˆ

φBˆ

φ,ˆr=Aˆ

θ,ˆrˆr−Aˆr,ˆ

θˆr+ (Γˆ

θˆrˆ

θAˆ

θ),ˆr

Bˆ

θ,ˆr=Aˆr, ˆ

φˆr−Aˆ

φ,ˆrˆr−(Γˆ

φˆrˆ

φAˆ

φ),ˆrBˆr,ˆ

θ=Aˆ

φ,ˆ

θˆ

θ−Aˆ

θ, ˆ

φˆ

θ+ (Γˆ

φˆ

θˆ

φAˆ

φ),ˆ

(339)

Thus,

Bˆα, ˆ

β= (Bˆα, ˆ

β)(0) +M(2curl2)

ˆαˆ

βˆγˆ

δAˆγ,ˆ

δ+M(1curl2)

ˆαˆ

βˆγAˆγ,(340)

where

(Bˆα,ˆ

δ)(0) =ǫˆαˆ

βˆγAˆγ, ˆ

βˆ

δ(341)

I.2 Differential operators 171

with

Ψ,ˆrˆr= Ψ,rr (342)

Ψ,ˆ

θˆ

θ= Ψ,θθ r−2(343)

Ψ,ˆ

φˆ

φ= Ψ,φφ r−2sin−2θ(344)

Ψ,ˆrˆ

θ= Ψ,rθ r−1(345)

Ψ,ˆ

θˆr= Ψ,θr r−1−Ψ,ˆ

θr−1(346)

Ψ,ˆrˆ

φ= Ψ,rφ r−1sin−1θ(347)

Ψ,ˆ

φˆr= Ψ,φr r−1sin−1θ−Ψ,ˆ

φr−1(348)

Ψ,ˆ

θˆ

φ= Ψ,θφ r−2sin−1θ(349)

and

Bˆ

φ,ˆ

θ=... + Γˆ

θˆrˆ

θAˆ

θ,ˆ

θ+ Γˆ

θˆrˆ

θ,ˆ

θAˆ

θBˆ

θ, ˆ

φ=... −Γˆ

φˆrˆ

φAˆ

φ,ˆ

φ−Γˆ

φˆrˆ

φ, ˆ

φAˆ

Bˆr, ˆ

φ=... + Γˆ

φˆ

θˆ

φAˆ

φ,ˆ

φ+ Γˆ

φˆ

θˆ

φ, ˆ

φAˆ

φBˆ

φ,ˆr=... + Γˆ

θˆrˆ

θAˆ

θ,ˆr+ Γˆ

θˆrˆ

θ,ˆrAˆ

Bˆ

θ,ˆr=... −Γˆ

φˆrˆ

φAˆ

φ,ˆr−Γˆ

φˆrˆ

φ,ˆrAˆ

φBˆr,ˆ

θ=... + Γˆ

φˆ

θˆ

φAˆ

φ,ˆ

θ+ Γˆ

φˆ

θˆ

φ,ˆ

θAˆ

(350)

Note that some derivatives of Christoffel symbols vanish, so we are left with

Bˆ

φ,ˆ

θ=... +r−1Aˆ

θ,ˆ

θBˆ

θ, ˆ

φ=... −r−1Aˆ

φ,ˆ

Bˆr, ˆ

φ=... +r−1cotθAˆ

φ,ˆ

φBˆ

φ,ˆr=... +r−1Aˆ

θ,ˆr−r−2Aˆ

Bˆ

θ,ˆr=... −r−1Aˆ

φ,ˆr+r−2Aˆ

φBˆr,ˆ

θ=... +r−1cotθ Aˆ

φ,ˆ

θ−r−2sin−2θ Aˆ

(351)

I.2.13 Gradient of a divergence

Aˆα; ˆαˆγ=Aˆα, ˆαˆγ−ΓˆσˆαˆαAˆσ,ˆγ−Γˆσˆαˆα,ˆγAˆσ−ΓˆσˆαˆγAˆσ, ˆα+ ΓˆσˆαˆγΓˆνˆσˆαAˆν−ΓˆσˆαˆγAˆα,ˆσ+ ΓˆσˆαˆγΓˆνˆαˆσAˆν.

ˆrcomponent:

Aˆα; ˆαˆr=Aˆα,ˆαˆr−ΓˆσˆαˆαAˆσ,ˆr−Γˆσˆαˆα,ˆrAˆσ−ΓˆσˆαˆrAˆσ,ˆα+ ΓˆσˆαˆrΓˆνˆσˆαAˆν−ΓˆσˆαˆrAˆα,ˆσ+ ΓˆσˆαˆrΓˆνˆαˆσAˆν

=Aˆα, ˆαˆr−ΓˆσˆαˆαAˆσ,ˆr−Γˆσˆαˆα,ˆrAˆσ

=Aˆα, ˆαˆr+ 2r−1Aˆr,ˆr+r−1cotθAˆ

θ,ˆr−2r−2Aˆr−r−2cotθAˆ

θ(352)

θcomponent:

Aˆα; ˆαˆ

θ=Aˆα, ˆαˆ

θ−ΓˆσˆαˆαAˆσ,ˆ

θ−Γˆσ

ˆαˆα,ˆ

θAˆσ−Γˆσ

ˆαˆ

θAˆσ, ˆα+ Γˆσ

ˆαˆ

θΓˆνˆσˆαAˆν−Γˆσ

ˆαˆ

θAˆα,ˆσ+ Γˆσ

ˆαˆ

θΓˆνˆαˆσAˆν

=Aˆα, ˆαˆ

θ+ 2r−1Aˆr,ˆ

θ+r−1cotθAˆ

θ,ˆ

θ−r−2sin−2θAˆ

θ(353)

Note that the last four terms in the above expression canceled, because

−Γˆσ

ˆαˆ

θAˆσ, ˆα+ Γˆσ

ˆαˆ

θΓˆνˆσˆαAˆν−Γˆσ

ˆαˆ

θAˆα,ˆσ+ Γˆσ

ˆαˆ

θΓˆνˆαˆσAˆν

=−r−1Aˆ

θ,ˆr+r−1Aˆr,ˆ

θ−r−2Aˆ

θ−r−1Aˆr,ˆ

θ+r−1Aˆ

θ,ˆr+r−2Aˆ

θ= 0 (354)

φcomponent:

Aˆα; ˆαˆ

φ=Aˆα, ˆαˆ

φ−ΓˆσˆαˆαAˆσ, ˆ

φ−Γˆσ

ˆαˆα, ˆ

φAˆσ−Γˆσ

ˆαˆ

φAˆσ, ˆα+ Γˆσ

ˆαˆ

φΓˆνˆσˆαAˆν−Γˆσ

ˆαˆ

φAˆα,ˆσ+ Γˆσ

ˆαˆ

φΓˆνˆαˆσAˆν.

=Aˆα, ˆαˆ

φ−ΓˆσˆαˆαAˆσ, ˆ

φ−Γˆσ

ˆαˆα, ˆ

φAˆσ

172 THE PENCIL CODE

=Aˆα, ˆαˆ

φ−ΓˆσˆαˆαAˆσ, ˆ

=Aˆα, ˆαˆ

φ−Γˆrˆ

θˆ

θAˆr, ˆ

φ−Γˆrˆ

φˆ

φAˆr, ˆ

φ−Γˆ

θˆ

φˆ

φAˆ

θ, ˆ

=Aˆα, ˆαˆ

φ+r−1Aˆr, ˆ

φ+r−1cotθAˆ

θ, ˆ

=Aˆα, ˆαˆ

φ+ 2r−1Aˆr, ˆ

φ+r−1cotθAˆ

θ, ˆ

φ(355)

In the ﬁrst line of the expression above, the last four terms vanish21 and the φderivative

of any Christoffel symbol (term before that) also vanishes.

21 The following four terms vanish because

−Γˆσ

ˆαˆ

φAˆσ, ˆα+ Γˆσ

ˆαˆ

φΓˆνˆσˆαAˆν−Γˆσ

ˆαˆ

φAˆα,ˆσ+ Γˆσ

ˆαˆ

φΓˆνˆαˆσAˆν

= Γˆσ

ˆαˆ

φ(−Aˆσ, ˆα+ ΓˆνˆσˆαAˆν−Aˆα,ˆσ+ ΓˆνˆαˆσAˆν)

= Γˆ

ˆrˆ

φ(−Aˆ

φ,ˆr+ Γˆνˆ

φˆrAˆν−Aˆr, ˆ

φ+ Γˆν

ˆrˆ

φAˆν)

+ Γˆrˆ

φˆ

φ(−Aˆr, ˆ

φ+ Γˆν

ˆrˆ

φAˆν−Aˆ

φ,ˆr+ Γˆνˆ

φˆrAˆν)

+ Γˆ

φˆ

θˆ

φ(−Aˆ

φ,ˆ

θ+ Γˆνˆ

φˆ

θAˆν−Aˆ

θ, ˆ

φ+ Γˆνˆ

θˆ

φAˆν)

+ Γˆ

θˆ

φˆ

φ(−Aˆ

θ, ˆ

φ+ Γˆνˆ

θˆ

φAˆν−Aˆ

φ,ˆ

θ+ Γˆνˆ

φˆ

θAˆν)

= Γˆ

ˆrˆ

φ(−Aˆ

φ,ˆr−Aˆr, ˆ

φ+ Γˆν

ˆrˆ

φAˆν)

+ Γˆrˆ

φˆ

φ(−Aˆr, ˆ

φ+ Γˆν

ˆrˆ

φAˆν−Aˆ

φ,ˆr)

+ Γˆ

φˆ

θˆ

φ(−Aˆ

φ,ˆ

θ−Aˆ

θ, ˆ

φ+ Γˆνˆ

θˆ

φAˆν)

+ Γˆ

θˆ

φˆ

φ(−Aˆ

θ, ˆ

φ+ Γˆνˆ

θˆ

φAˆν−Aˆ

φ,ˆ

θ)

=r−1(−Aˆ

φ,ˆr−Aˆr, ˆ

φ+ Γˆν

ˆrˆ

φAˆν)

−r−1(−Aˆr, ˆ

φ−Aˆ

φ,ˆr+ Γˆν

ˆrˆ

φAˆν)

+r−1cotθ(−Aˆ

φ,ˆ

θ−Aˆ

θ, ˆ

φ+ Γˆνˆ

θˆ

φAˆν)

−r−1cotθ(−Aˆ

θ, ˆ

φ−Aˆ

φ,ˆ

θ+ Γˆνˆ

θˆ

φAˆν) = 0 (356)

J. Switchable modules 173

J Switchable modules

The material in this section is being assembled from the ﬁle ‘inlinedoc-modules.tex’,

which is automatically assembled. However, it is currently incomplete and contains only

a small number of the available modules.

Module Description

hydro.f90

This module takes care of most of the things related to velocity.

Pressure, for example, is added in the energy (entropy) module.

chemistry.f90

This modules adds chemical species and reactions.

The units used in the chem.in ﬁles are cm3,mole,sec,kcal and K

gpu astaroth.f90

This module contains GPU related types and functions to be used with

ASTAROTH nucleus.

noentropy.f90

Calculates pressure gradient term for

polytropic equation of state p=constρΓ.

nogpu.f90

This module contains GPU related dummy types and functions.

nohydro.f90

no variable u: useful for kinematic dynamo runs.

nopower spectrum.f90

reads in full snapshot and calculates power spetrum of u

noyinyang.f90

This module contains Yin-Yang related dummy types and functions.

noyinyang mpi.f90

This module contains Yin-Yang related dummy types and functions.

particles adsorbed.f90

This module takes care of the evolution of adsorbed

species on the particle surface for reactive particles

particles chemistry.f90

This module implements reactive particles.

particles surfspec.f90

immediate vicinity of reactive particles.

power spectrum.f90

reads in full snapshot and calculates power spetrum of u

test chemistry.f90

This modules adds chemical species and reactions.

The units used in the chem.in ﬁles are cm3,mole,sec,kcal and K

timestep.f90

Runge-Kutta time advance, accurate to order itorder.

At the moment, itorder can be 1, 2, or 3.

timestep strang.f90

Runge-Kutta time advance, accurate to order itorder.

At the moment, itorder can be 1, 2, or 3.

timestep subcycle.f90

This is a highly speciﬁed timestep module currently only working

together with the special module coronae.f90.

yinyang.f90

This module contains Yin-Yang related types and functions

which are incompatible with FORTRAN 95.

yinyang mpi.f90

This module contains Yin-Yang related types and functions

which are incompatible with FORTRAN 95.

174 THE PENCIL CODE

K Startup and run-time parameters

K.1 List of startup parameters for ‘start.in’

The following table lists all (at the time of writing, September 2002) namelists used

in ‘start.in’, with the corresponding parameters and their default values (in square

brackets). Any variable referred to as a

ﬂag

can be set to any nonzero value to switch

the corresponding feature on. Not all parameters are used for a given scenario. This

list is not necessarily up to date; also, in many cases it can only give an idea of the

corresponding initial state; to get more insight and the latest set of parameters, you

need to look at the code.

The value εcorresponds to 5 times the smallest number larger than zero. For single

precision, this is typically about ε≈5×1.2×10−7= 6×10−7; for double precision, ε≈

10−15.

Variable [default value] Meaning

Namelist

init pars

cvsid

[’’] the

svn

identiﬁcation string, which allows you to

keep track of the version of ‘start.in’.

[14] (anti-)verbosity level: ip=1 produces lots of diagnos-

tic output, ip=14 virtually none.

xyz0

[(−π, −π, −π)],

Lxyz

[(2π, 2π, 2π)],

lperi

[(T,T,T)] determine the geometry of the box. All three are vec-

tors of the form (x-comp., y-comp., z-comp.);

xyz0

de-

scribes the left (lower) corner of the box,

Lxyz

the box

size.

lperi

speciﬁes whether a direction is considered

periodic (in which case the last point is omitted) or

not. In all cases, three ghost zones will be added.

lprocz slowest

[T] if set to F, the ordering of processor numbers is

changed, so the zprocessors are now in the inner

loop. Since

nprocy

=4 is optimal (see Sect. 5.20.2),

you may want to put

lprocz slowest

=T when

nygrid>nzgrid.

lwrite ic

[F] if set T, the initial data are written into the ﬁle ‘VAR0’.

This is generally useful, but doing this all the time

uses up plenty of disk space.

lnowrite

[F] if set T, all initialization ﬁles are written, including

the param.nml ﬁle, except ‘var.dat’. This option al-

lows you to use old ﬁlevar.dat ﬁles, but updates all

other initialization ﬁles. This could be useful after

having changed the code and, in particular, when the

‘var.dat’ ﬁles will be overwritten by ‘remesh.csh’.

lwrite aux

[F] if set T, auxiliary variables (those calculated at each

step, but not evolved mathematically) to ‘var.dat’ af-

ter the evolved quantities.

lwrite 2d

[F] if set T, only 2D-snapshots are written into VAR ﬁles

in the case of 2D-runs with nygrid = 1 or nzgrid = 1.

K.1 Startup parameters for ‘start.in’ 175

lread oldsnap

[F] if set T, the old snapshot will be read in before pro-

ducing (overwriting) initial conditions. For example,

if you just want to add a perturbation to the mag-

netic ﬁeld, you’d give no initial condition for density

and velocity (so you keep the data from a hopefully

relaxed run), and just add whatever you need for the

magnetic ﬁeld. In this connection you may want to

touch NOERASE, so as not to erase the previous data.

lread oldsnap nomag

[F] if set T, the old snapshot from a non-magnetic run

will be read in before producing (overwriting) ini-

tial conditions. This allows one to let a hydrody-

namic run relax before adding a magnetic ﬁeld.

However, for this to work one has to modify manu-

ally ‘data/param.nml’ by adding an entry for

MAG-

NETIC INIT PARS

PSCALAR INIT PARS

. In

addition, for idl to read correctly after the ﬁrst

restarted run, you must adjust the value of

mvar

‘data/dim.dat’

lread oldsnap nopscalar

[F] if set T, the old snapshot from a run without passive

scalar will be read in before producing (overwriting)

initial conditions. This allows one to let a hydrody-

namic run relax before adding a passive scalar.

lshift origin

[F,F,F] if set Tfor any or some of the three directions, the

mesh is shifted by 1/2 meshpoint in that or those di-

rections so that the mesh goes through the origin.

unit system

[’cgs’] you can set this character string to ’SI’, which

means that you can give physical dimensions in SI

units. The default is cgs units.

unit length

[1] allows you to set the unit length. Suppose you want

the unit length to be 1 kpc, then you would say unit_-

length=’3e21’. (Of course, politically correct would

be to say unit_system=’SI’ in which case you say

unit_length=’3e19’.)

unit velocity

[1] Example: if you want km/s you say unit_-

length=’1e5’.

unit density

[1] Example: if you want your unit density to be

10−24 g/cm3you say unit_density=’1e-24’.

unit temperature

[1] Example: unit_temperature=’1e6’ if you want mega-

Kelvin.

random gen

[system] choose random number generator; currently valid

choices are

’system’ (your compiler’s generator),

’min_std’ (the ‘minimal standard’ generator ran0()

from ‘Numerical Recipes’),

’nr_f90’ (the Parker-Miller-Marsaglia generator

ran() from ‘Numerical Recipes for F90’).

bcx

[(’p’,’p’, . . . )],

bcy

[(’p’,’p’, . . . )],

176 THE PENCIL CODE

bcz

[(’p’,’p’, . . . )] boundary conditions. See Sect. 5.16 for a discussion

of where and how to set these.

pretend lnTT

[F] selects ln Tas fundamental thermodynamic variable

in the entropy module

Namelist

hydro init pars

inituu

[’zero’] initialization of velocity. Currently valid choices are

‘zero’ (u= 0 ),

‘gaussian-noise’ (random, normally-distributed

ux,uz),

‘gaussian-noise-x’ (random, normally-distributed

ux),

‘sound-wave’ (sound wave in xdirection),

‘shock-tube’ (polytropic standing shock),

‘bullets’ (blob-like velocity perturbations),

‘Alfven-circ-x’ (circularly polarized Alfven wave

in x direction),

‘const-ux’ (constant x-velocity),

‘const-uy’ (constant y-velocity),

‘tang-discont-z’ (tangential discontinuity: veloc-

ity is directed along x, jump is at z= 0),

‘Fourier-trunc’ (truncated Fourier series),

‘up-down’ (ﬂow upward in one spot, downward in

another; not solenoidal).

ampluu

[0.] amplitude for some types of initial velocities.

widthuu

[0.1] width for some types of initial velocities.

urand

[0.] additional random perturbation of u. If urand>0, the

perturbation is additive, ui7→ ui+urandU[0.5,0.5]; if

urand<0, it is multiplicative, ui7→ ui×urandU[0.5,0.5]; in

both cases, U[0.5,0.5] is a uniformly distributed random

variable on the interval [−0.5,0.5].

uu left

[0.],

uu right

[0.] needed for inituu=’shock-tube’.

Namelist

density init pars

K.1 Startup parameters for ‘start.in’ 177

initlnrho

[’zero’] initialization of density. Currently valid choices are

‘zero’ (ln ρ= 0),

‘isothermal’ (isothermal stratiﬁcation),

‘polytropic_simple’ (polytropic stratiﬁcation),

‘hydrostatic-z-2’ (hydrostatic vertical stratiﬁca-

tion for isentropic atmosphere),

‘xjump’ (density jump in xof width

widthlnrho

‘rho-jump-z’ (density jump in zof width

widthlnrho

‘piecew-poly’ (piecewise polytropic vertical strati-

ﬁcation for solar convection),

‘polytropic’ (polytropic vertical stratiﬁcation),

‘sound-wave’ (sound wave),

‘shock-tube’ (polytropic standing shock),

‘gaussian-noise’ (Gaussian-distributed, uncorre-

lated noise),

‘gaussian-noise’ (Gaussian-distributed, uncorre-

lated noise in x, but uniform in yand z),

‘hydrostatic-r’ (hydrostatic radial density strati-

ﬁcation for isentropic or isothermal sphere),

‘sin-xy’ (sine proﬁle in xand y),

‘sin-xy-rho’ (sine proﬁle in xand y, but in ρ, not

ln ρ),

‘linear’ (linear proﬁle in k·x),

‘planet’ (planet solution; see §C.7).

gamma

[5./3] adiabatic index γ=cp/cv.

cs0

[1.] can be used to set the dimension of velocity; larger

values can be used to decrease stratiﬁcation

rho0

[1.] reference values of sound speed and density, i. e. val-

ues at height

zref

ampllnrho

[0.],

widthlnrho

[0.1] amplitude and width for some types of initial densi-

ties.

rho left

[1.],

rho right

[1.] needed for initlnrho=’shock-tube’.

cs2bot

[1.],

cs2top

[1.] sound speed at bottom and top. Needed for some

types of stratiﬁcation.

Namelist

grav init pars

zref

[0.] reference height where in the initial stratiﬁcation

s=c2

s0 and ln ρ= ln ρ0.

gravz

[−1.] vertical gravity component gz.

grav proﬁle

[’const’] constant gravity gz=gravz (grav_profile=’const’)

gravity or linear proﬁle gz=gravz ·z(grav_-

profile=’linear’, for accretion discs and similar).

[0.],

178 THE PENCIL CODE

[1.] speciﬁc to the solar convection case

initlnrho=’piecew-poly’. The stable layer is

z0< z < z1, the unstable layer z1< z < z2, and the

top (isothermal) layer is z2< z < ztop.

nu epicycle

[1.] vertical epicyclic frequency; for accretion discs it

should be equal to Omega, but not for galactic discs;

see Eq. (135) in Sect. C.5.

grav amp

[0.],

grav tilt

[0.] speciﬁc to the tilted gravity case (amplitude and an-

gle wrt the vertical direction).

Namelist

entropy init pars

initss

[’nothing’] initialization of entropy. Currently valid choices are

‘nothing’ (leaves the initialization done in the den-

sity module unchanged),

‘zero’ (put s= 0 explicitly; this may overwrite the

initialization done in the density module),

‘isothermal’ (isothermal stratiﬁcation, T=const),

‘isobaric’ (isobaric, p=const),

‘isentropic’ (isentropic with superimposed hot [or

cool] bubble),

‘linprof’ (linear entropy proﬁle in z),

‘piecew-poly’ (piecewise polytropic stratiﬁcation

for convection),

‘polytropic’ (polytropic stratiﬁcation, polytropic

exponent is

mpoly0

‘blob’ (puts a gaussian blob in entropy for buoy-

ancy experiments; see Ref. [7] for details)

‘xjump’ (jump in xdirection),

‘hor-tube’ (horizontal ﬂux tube in entropy, ori-

ented in the y-direction).

pertss

[’zero’] additional perturbation to entropy. Currently valid

choices are

’zero’ (no perturbation)

’hexagonal’ (hexagonal perturbation for convec-

tion).

ampl ss

[0.],

widthss

[2ε] amplitude and width for some types of initial en-

tropy.

grads0

[0.] initial entropy gradient for initss=linprof.

radius ss

[0.1] radius of bubble for initss=isentropic.

mpoly0

[1.5],

mpoly1

[1.5],

K.1 Startup parameters for ‘start.in’ 179

mpoly2

[1.5] speciﬁc to the solar convection case

initss=piecew-poly: polytropic indices of unstable

(

mpoly0

), stable (

mpoly1

) and top layer (

mpoly2

). If

the ﬂag

isothtop

is set, the top layer is initialized to

be isothermal, otherwise thermal (plus hydrostatic)

equilibrium is assumed for all three layers, which

results in a piecewise polytropic stratiﬁcation.

isothtop

[0] ﬂag for isothermal top layer for initss=piecew-poly.

khor ss

[1.] horizontal wave number for pertss=hexagonal

Namelist

magnetic init pars

initaa

[’zero’] initialization of magnetic ﬁeld (vector potential).

Currently valid choices are

‘Alfven-x’ (Alfv´

en wave traveling in the x-

direction; this also sets the velocity),

‘Alfven-z’ (Alfv´

en wave traveling in the z-

direction; this also sets the velocity),

‘Alfvenz-rot’ (same as ‘Alfven-z’, but with rota-

tion),

‘Alfven-circ-x’ (circularly polarized Alfven wave

in x direction),

‘Beltrami-x’ (x-dependent Beltrami wave),

‘Beltrami-y’ (y-dependent Beltrami wave),

‘Beltrami-z’ (z-dependent Beltrami wave),

‘Bz(x)’ (Bz∝cos(kx)),

‘crazy’ (for testing purposes).

‘diffrot’ ([needs to be documented]),

‘fluxrings’ (two interlocked magnetic ﬂuxrings;

see §C.4),

‘gaussian-noise’ (white noise),

‘halfcos-Bx’ ([needs to be documented]),

‘hor-tube’ (horizontal ﬂux tube in B, oriented in

the y-direction).

‘hor-fluxlayer’ (horizontal ﬂux layer),

‘mag-support’ ([needs to be documented]),

‘mode’ ([needs to be documented]),

‘modeb’ ([needs to be documented]),

‘propto-ux’ ([needs to be documented]),

‘propto-uy’ ([needs to be documented]),

‘propto-uz’ ([needs to be documented]),

‘sinxsinz’ (sin xsin z),

‘uniform-Bx’ (uniform ﬁeld in xdirection),

‘uniform-By’ (uniform ﬁeld in ydirection),

‘uniform-Bz’ (uniform ﬁeld in zdirection),

‘zero’ (zero ﬁeld),

180 THE PENCIL CODE

initaa2

[’zero’] additional perturbation of magnetic ﬁeld. Currently

valid choices are

‘zero’ (zero perturbation),

‘Beltrami-x’ (x-dependent Beltrami wave),

‘Beltrami-y’ (y-dependent Beltrami wave),

‘Beltrami-z’ (z-dependent Beltrami wave).

amplaa

[0.] amplitude for some types of initial magnetic ﬁelds.

amplaa2

[0.] amplitude for some types of magnetic ﬁeld perturba-

tion.

fring

{

1,2

}[0.],

Iring

{

1,2

}[0.],

Rring

{

1,2

}[1.],

{

1,2

}[0.3] ﬂux, current, outer and inner radius of ﬂux ring 1/2;

see Sect. C.4.

radius

[0.1] used by some initial ﬁelds.

epsilonaa

[10−2] used by some initial ﬁelds.

widthaa

[0.5] used by some initial ﬁelds.

z0aa

[0.] used by some initial ﬁelds.

kx aa

[1.],

ky aa

[1.],

kz aa

[1.] wavenumbers used by some initial ﬁelds.

lpress equil

[F] ﬂag for pressure equilibrium (can be used in connec-

tion with all initial ﬁelds)

Namelist

pscalar init pars

initlncc

[’zero’] initialization of passive scalar (concentration per

unit mass, c). Currently valid choices (for ln c) are

‘zero’ (ln c= 0.),

‘gaussian-noise’ (white noise),

‘wave-x’ (wave in xdirection),

‘wave-y’ (wave in ydirection),

‘wave-z’ (wave in zdirection),

‘tang-discont-z’ (Kelvin-Helmholtz instability),

‘hor-tube’ (horizontal tube in concentration; used

as a marker for magnetic ﬂux tubes).

initlncc2

[’zero’] additional perturbation of passive scalar concentra-

tion c. Currently valid choices are

‘zero’ (δln c= 0.),

‘wave-x’ (add x-directed wave to ln c).

ampllncc

[0.1] amplitude for some types of initial concentration.

ampllncc2

[0.] amplitude for some types of concentration perturba-

tion.

kx lncc

[1.],

ky lncc

[1.],

kz lncc

[1.] wave numbers for some types of initial concentra-

tion.

Namelist

shear init pars

K.2 Runtime parameters for ‘run.in’ 181

qshear

[0.] degree of shear for shearing-box simulations (the

shearing-periodic boundaries are the x-boundaries

and are sheared in the y-direction). The shear veloc-

ity is U=−qΩx ˆ

Namelist

particles ads init pars

init ads mol frac

[0.] initial adsorbed mole fraction

Namelist

particles surf init pars

init surf mol frac

[0.] initial surface mole fraction

Namelist

particles chem init pars

total carbon sites

[1.08e−8] carbon sites per surface area [mol/cm]2

Namelist

particles stalker init pars

dstalk

[0.1] times between printout of stalker data

lstalk xx

[F] particles position

lstalk vv

[F] particles velocity

lstalk uu

[F] gas velocity at particles position

lstalk guu

[F] gas velocity gradient at particles position

lstalk rho

[F] gas density at particles position

lstalk grho

[F] gas density gradient at particles position

lstalk ap

[F] particles diameter

lstalk bb

[T] magnetic ﬁeld at particles position

lstalk relvel

[F] particles relative velocity to gas

K.2 List of runtime parameters for ‘run.in’

The following table lists all (at the time of writing, September 2002) namelists used

in ﬁle ‘run.in’, with the corresponding parameters and their default values (in square

brackets). Default values marked as [start] are taken from ‘start.in’. Any variable re-

ferred to as a

ﬂag

can be set to any nonzero value to switch the corresponding feature

on. Not all parameters are used for a given scenario. This list is not necessarily up to

date; also, in many cases it can only give an idea of the corresponding setup; to get more

insight and the latest set of parameters, you need to look at the code.

Once you have changed any of the ‘*.in’ ﬁles, you may want to ﬁrst execute the command

pc_configtest in order to test the correctness of these conﬁguration ﬁles, before you

apply them in an active simulation run.

Variable [default value] Meaning

Namelist

run pars

cvsid

[’’]

svn

identiﬁcation string, which allows you to keep

track of the version of ‘run.in’.

[14] (anti-)verbosity level: ip=1 produces lots of addi-

tional diagnostic output, ip=14 virtually none.

[0] number of time steps to run. This number can be

increased or decreased during the run by touch

RELOAD.

182 THE PENCIL CODE

it1

[10] write diagnostic output every

it1

time steps (see

Sect. 5.5).

it1d

[it1] write averages every

it1d

time steps (see Sect. 5.8.1).

it1d

has to be greater than or equal to

it1

cdt

[0.9] Courant coefﬁcient for advective time step; see §5.15.

cdtv

[0.25] Courant coefﬁcient for diffusive time step; see §5.15.

[0.] time step; if 6= 0., this overwrites the Courant time

step. See §5.15 for a discussion of the latter.

dtmin

[10−6] abort if time step δt < δtmin.

tmax

[1033] don’t run time steps beyond this time. Useful if you

want to run for a given amount of time, but don’t

know the necessary number of time steps.

isave

[100] update current snapshot ‘var.dat’ every

isave

time

steps.

itorder

[3] order of time step (1 for Euler; 2 for 3nd-order, 3 for

3rd-order Runge–Kutta).

dsnap

[100.] save permanent snapshot every

dsnap

time units

to ﬁles ‘VARN’, where Ncounts from N= 1

upward. (This information is stored in the ﬁle

‘data/tsnap.dat’; see the module

wsnaps.f90

, which

in turn uses the subroutines

out1

and

out2

dvid

[100.] write two-dimensional sections for generation of

videos every

dvid

time units (not timesteps; see the

subroutines

out1

and

out2

in the code).

iwig

[0] if 6= 0, apply a Nyquist ﬁlter (a ﬁlter eliminating any

signal at the Nyquist frequency, but affecting large

scales as little as possible) every

iwig

time steps to

logarithmic density (sometimes necessary with con-

vection simulations).

[−1],

iz2

[−1] position of slice planes for video ﬁles. Any negative

value of some of these variables will be overwritten

according to the value of

slice position

. See §5.7) for

details.

slice position

[’p’] symbolic speciﬁcation of slice position. Currently

valid choices are

’p’ (periphery of the box)

’m’ (middle of the box)

’e’ (equator for half-sphere calculations, i. e. x,y

centered, zbottom)

These settings are overridden by explicitly setting

iz2

. See §5.7) for details.

zbot slice

[value] z position of slice xy-plane. The value can be any ﬂoat

number inside the z domain. These settings are over-

ridden by explicitly setting

iz2

. Saved as

slice with the sufﬁx

. See §5.7) for details.

ztop slice

[value] z position of slice xy-plane. The value can be any ﬂoat

number inside the z domain. These settings are over-

ridden by explicitly setting

iz2

. Saved as

slice with the sufﬁx

xy2

. See §5.7) for details.

K.2 Runtime parameters for ‘run.in’ 183

tavg

[0] averaging time τavg for time averages (if 6= 0); at the

same time, time interval for writing time averages.

See §5.8.4 for details.

idx tavg

[(0,0,...,0)] indices of variables to time-average. See §5.8.4 for

details.

d2davg

[100.] time interval for azimuthal and z-averages, i.e. the

averages that produce 2d data. See §5.8.3 for details.

ialive

[0] if 6= 0, each processor writes the current time step

to ‘alive.info’ every

ialive

time steps. This provides

the best test that the job is still alive. (This can be

used to ﬁnd out which node has crashed if there is a

problem and the run is hanging.)

bcx

[(’p’,’p’, . . . )],

bcy

[(’p’,’p’, . . . )],

bcz

[(’p’,’p’, . . . )] boundary conditions. See Sect. 5.16 for a discussion

of where and how to set these.

random gen

[start] see start parameters, p. 175

lwrite aux

[start] if set T, auxiliary variables (those calculated at each

step, but not evolved mathematically) to ‘var.dat’

and ‘VAR’ ﬁles after the evolved quantities.

Namelist

hydro run pars

Omega

[0.] magnitude of angular velocity for

Coriolis force

(note: the centrifugal force is turned off by default,

unless lcentrifugal_force=T is set).

theta

[0.] direction of angular velocity in degrees (θ= 0 for z-

direction, θ= 90 for the negative x-direction, corre-

sponding to a box located at the equator of a rotating

sphere. Thus, e.g., θ= 60 corresponds to 30◦latitude.

(Note: prior to April 29, 2007, there was a minus sign

in the deﬁnition of θ.)

ttransient

[0.] initial time span for which to do something special

(transient). Currently just used to smoothly switch

on heating [Should be in

run pars

, rather than here].

dampu

[0.],

tdamp

[0.],

ldamp fade

[F] damp motions during the initial time interval 0< t <

tdamp with a damping term −

dampu

(u). If

ldamp -

fade

is set, smoothly reduce damping to zero over

the second half of the time interval

tdamp

. Initial ve-

locity damping is useful for situations where initial

conditions are far from equilibrium.

dampuint

[0.], weighting of damping external to spherical region

(see

wdamp

damp

ubelow).

dampuext

[0.], weighting of damping in internal spherical region

(see

wdamp

damp

ubelow).

rdampint

[0.], radius of internal damping region

rdampext

[impossible], radius of external damping region, used in place of

former variable

rdamp

184 THE PENCIL CODE

wdamp

[0.2], permanently damp motions in |x|< rdampint

with damping term −

damp

uint uχ(r−rdampint)

or |x|> rdampext with damping term

−

damp

uext uχ(r−rdampext), where χ(·)is a smooth

proﬁle of width

wdamp

ampl forc

[0.], amplitude of the ux-forcing or uy-forcing on the verti-

cal boundaries that is of the form ux(t) = ampl forc∗

sin(kforc ∗x)∗cos(w forc ∗t)[must be used in

connection with bcx=’g’ or bcz=‘g’ and force lower -

bound=‘vel time’ or force upper bound=‘vel time’]

k forc

[0.], corresponding horizontal wavenumber

w forc

[0.] corresponding frequency

Namelist

density run pars

cs0

[start],

rho0

[start],

gamma

[start] see start parameters, p. 177

cdiffrho

[0.] Coefﬁcient for mass diffusion (diffusion term will be

cdiﬀrho δx cs0.

cs2bot

[start],

cs2top

[start] squared sound speed at bottom and top for boundary

condition ‘c2’.

lupw lnrho

[.false.] use 5th-order upwind derivative operator for the ad-

vection term u·∇ln ρto avoid spurious Nyquist sig-

nal (‘wiggles’); see §H.2.

Namelist

entropy run pars

hcond0

[0.],

hcond1

[start],

hcond2

[start] speciﬁc to the solar convection case

initss=piecew-poly: heat conductivities Kin

the individual layers.

hcond0

is the value Kunst in

the unstable layer,

hcond1

is the ratio Kstab/Kunst for

the stable layer, and

hcond2

is the ratio Ktop/Kunst

for the top layer. The function K(z)is not discontin-

uous, as the transition between the different values

is smoothed over the width

widthss

. If

hcond1

hcond2

are not set, they are calculated according to

the polytropic indices of the initial proﬁle, K∝m+1.

iheatcond

[’K-const’] select type of heat conduction. Currently valid

choices are

‘K-const’ (constant heat conductivity),

‘K-profile’ (vertical or radial proﬁle),

‘chi-const’ (constant thermal diffusivity),

‘magnetic’ (heat conduction by electrons in mag-

netic ﬁeld – currently still experimental).

lcalc heatcond constchi

[F] ﬂag for assuming thermal diffusivity χ=K/(cpρ) =

const, rather than K=const (which is the

default). This is currently only correct with

‘noionization.f90’. Superseded by

iheatcond

K.2 Runtime parameters for ‘run.in’ 185

chi

[0.] value of χwhen lcalc_heatcond_constchi=T.

widthss

[start] width of transition region between layers. See start

parameters, p. 179.

isothtop

[start] ﬂag for isothermal top layer for solar convection case.

See start parameters, p. 179.

luminosity

[0.],

wheat

[0.1] strength and width of heating region.

cooltype

[’Temp’] type of cooling; currently only implemented for spher-

ical geometry. Currently valid choices are

‘Temp’,‘cs2’ (cool temperature toward c2

cs2cool

) with a cooling term

−C =−ccool

s−c2

scool

)

‘Temp-rho’,cs2-rho (cool temperature toward c2

cs2cool

) with a cooling term

−C =−ccool ρc2

s−c2

scool

— this avoids numerical instabilities in low-

density regions [currently, the cooling coefﬁ-

cient ccool ≡

cool

is not taken into account when

the time step is calculated])

‘entropy’ (cool entropy toward 0.).

cool

[0.],

wcool

[0.1] strength ccool and smoothing width of cooling region.

rcool

[1.] radius of cooling region: cool for |x| ≥

rcool

Fbot

[start] heat ﬂux for bottom boundary condition ‘c1’. For

polytropic atmospheres, if

Fbot

is not set, it will be

calculated from the value of

hcond0

in ‘start.x’, pro-

vided the entropy boundary condition is set to ‘c1’.

chi t

[0.] entropy diffusion coefﬁcient for diffusive term

∂s/∂t =...+χt∇2sin the entropy equation, that can

represent some kind of turbulent (sub-grid) mixing.

It is probably a bad idea to combine this with heat

conduction

hcond0

6= 0.

lupw ss

[.false.] use 5th-order upwind derivative operator for the ad-

vection term u·∇sto avoid spurious Nyquist signal

(‘wiggles’); see §H.2.

tauheat buffer

[0.] time scale for heating to target temperature

TTheat buffer

); zero disables the buffer zone.

zheat buffer

[0.]zcoordinate of the thermal buffer zone. Buffering is

active in |z|>

TTheat buffer

dheat buffer1

[0.] Inverse thickness of transition to buffered layer.

TTheat buffer

[0.] target temperature in thermal buffer zone (zdirec-

tion only).

186 THE PENCIL CODE

lhcond global

[F] ﬂag for calculating the heat conductivity K(and

also ∇log K) globally using the global arrays facility.

Only valid when

iheatcond

=‘K-profile’.

Namelist

magnetic run pars

B ext

[(0., 0., 0.)] uniform background magnetic ﬁeld (for fully periodic

boundary conditions, uniform ﬁelds need to be explic-

itly added, since otherwise the vector potential Ahas

a linear x-dependence which is incompatible with pe-

riodicity).

lignore Bext in b2

[F] add uniform background magnetic ﬁeld when

luse Bext in b2

[T] computing b2pencils

eta

[0.] magnetic diffusivity η= 1/(µ0σ), where σis the elec-

tric conductivity.

height eta

[0.],

eta out

[0.] used to add extra diffusivity in a halo region.

eta int

[0.] used to add extra diffusivity inside sphere of radius

r int

eta ext

[0.] used to add extra diffusivity outside sphere of radius

r ext

kinﬂow

[’’] set type of ﬂow ﬁxed with ‘nohydro’. Currently the

only recognized value is ’ABC’ for an ABC ﬂow; all

other values lead to u=0.

[1.],

[1.] wave numbers for ABC ﬂow.

ABC A

[1.],

ABC B

[1.],

ABC C

[1.] amplitudes A,Band Cfor ABC ﬂow.

Namelist

pscalar run pars

pscalar diff

[0.] diffusion for passive scalar concentration c.

tensor pscalar diff

[0.] coefﬁcient for non-isotropic diffusion of passive

scalar.

reinitialize lncc

[F] reinitialize the passive scalar to the value of cc const

in start.in at next run

Namelist

forcing run pars

iforce

[2] select form of forcing in the equation of motion; cur-

rently valid choices are

’zero’ (no forcing),

’irrotational’ (irrotational forcing),

’helical’ (helical forcing),

’fountain’ (forcing of “fountain ﬂow”; see Ref. [13]),

’horizontal-shear’ (forcing localized horizontal si-

nusoidal shear).

’variable_gravz’ (time-dependent vertical gravity

for forcing internal waves),

iforce2

[0] select form of additional forcing in the equation of

motion; valid choices are as for

iforce

K.2 Runtime parameters for ‘run.in’ 187

force

[0.] amplitude of forcing.

relhel

[1.] helicity of forcing. The parameter

relhel

corresponds

to σintroduced in Sect. G.2. (σ=±1corresponds to

maximum helicity of either sign).

height ff

[0.] multiply forcing by z-dependent proﬁle of width

height ff

(if 6= 0) .

r ff

[0.] if 6= 0, multiply forcing by spherical cutoff proﬁle (of

radius

r ff

) and ﬂip signs of helicity at equatorial

plane.

width ff

[0.5] width of vertical and radial proﬁles for modifying

forcing.

kfountain

[5] horizontal wavenumber of the fountain ﬂow.

fountain

[1.] amplitude of the fountain ﬂow.

omega ff

[1.] frequency of the cos or sin forcing [e.g. cos(omega -

ff*t)].

ampl ff

[1.] amplitude of forcing in front of cos or sin [e.g. ampl -

ff*cos(omega ff*t)].

Namelist

grav run pars

zref

[start],

gravz

[start],

grav proﬁle

[start] see p. 177.

nu epicycle

[start] see Eq. (135) in Sect. C.5.

Namelist

viscosity run pars

[0.] kinematic viscosity.

nu hyper2

[0.] kinematic hyperviscosity (with ∇4u).

nu hyper3

[0.] kinematic hyperviscosity (with ∇6u).

zeta

[0.] bulk viscosity.

ivisc

[’nu-const’] select form of viscous term (see §6.2); currently valid

choices are

’nu-const’ – viscous force for ν=const, Fvisc =

ν(∇2u+1

3∇∇ ·u+ 2S·∇ln ρ)

’rho_nu-const’ – viscous force for µ≡ρν =const,

Fvisc = (µ/ρ)(∇2u+1

3∇∇ ·u). With this op-

tion, the input parameter

actually sets the

value of µ/ρ0(

rho0

=ρ0is another input param-

eter, see pp. 177 and 184)

’simplified’ – simpliﬁed viscous force Fvisc =

ν∇2u

Namelist

shear run pars

qshear

[start] See p. 181.

Namelist

particles run pars

ldragforce dust par

[F] dragforce on particles

ldragforce gas par

[F] particle-gas friction force

ldraglaw steadystate

[F] particle forces only with 1

τ∆v

lpscalar sink

[F] particles consume passive scalar

pscalar sink rate

[0] volumetric pscalar consumption rate

188 THE PENCIL CODE

lbubble

[F] addition of the virtual mass term

Namelist

particles ads run pars

placeholder

[start] placeholder

Namelist

particles surf run pars

lspecies transfer [T]

Species transfer from solid to ﬂuid phase

Namelist

particles chem run pars

lthiele [T]

Modeling of particle porosity by application of Thiele

modulus

K.3 List of parameters for ‘print.in’

The following table lists all possible inputs to the ﬁle ‘print.in’ that are documented.

Variable Meaning

Module ‘cdata.f90’

number of time step (since beginning of job only)

time t(since start.csh)

time step δt

walltime

wall clock time since start of run.x, in seconds

Rmesh

Rmesh3

R(3)

mesh

maxadvec

Module ‘hydro.f90’

u2tm

Du(t)·Rt

0u(t′)dt′E

uotm

Du(t)·Rt

0ω(t′)dt′E

outm

Dω(t)·Rt

0u(t′)dt′E

fkinzm

1

2̺u2uz

u2m

hu2i

uxpt

ux(x1, y1, z1, t)

uypt

uy(x1, y1, z1, t)

uzpt

uz(x1, y1, z1, t)

uxp2

ux(x2, y2, z2, t)

uyp2

uy(x2, y2, z2, t)

uzp2

uz(x2, y2, z2, t)

urms

hu2i1/2

urmsx

hu2i1/2for the hydro xaver range

urmsz

hu2i1/2for the hydro zaver range

durms

hδu2i1/2

umax

max(|u|)

umin

min(|u|)

uxrms

hu2

xi1/2

uyrms

u2

y1/2

K.3 Parameters for ‘print.in’ 189

uzrms

hu2

zi1/2

uxmin

min(|ux|)

uymin

min(|uy|)

uzmin

min(|uz|)

uxmax

max(|ux|)

uymax

max(|uy|)

uzmax

max(|uz|)

uxm

huxi

uym

huyi

uzm

huzi

ux2m

hu2

uy2m

u2

y

uz2m

hu2

ux2ccm

hu2

xcos2kzi

ux2ssm

u2

xsin2kz

uy2ccm

u2

ycos2kz

uy2ssm

u2

ysin2kz

uxuycsm

huxuycos kz sin kzi

uxuym

huxuyi

uxuzm

huxuzi

uyuzm

huyuzi

umx

huxi

umy

huyi

umz

huzi

omumz

DhWixy · hUixyE(xy-averaged mean cross helicity produc-

tion)

umamz

Dhuixy · hAixyE

umbmz

DhUixy · hBixyE(xy-averaged mean cross helicity produc-

tion)

umxbmz

DhUixy × hBixyEz(xy-averaged mean emf)

rux2m

hρu2

ruy2m

ρu2

y

ruz2m

hρu2

divum

hdivu)i

rdivum

h̺divu)i

divu2m

h(divu)2i

gdivu2m

h(grad divu)2i

u3u21m

hu3u2,1i

u1u32m

hu1u3,2i

u2u13m

hu2u1,3i

u2u31m

hu2u3,1i

u3u12m

hu3u1,2i

u1u23m

hu1u2,3i

ruxm

h̺uxi(mean x-momentum density)

ruym

h̺uyi(mean y-momentum density)

ruzm

h̺uzi(mean z-momentum density)

ruxtot

hρ|u|i (mean absolute x-momentum density)

rumax

max(̺|u|)(maximum modulus of momentum)

190 THE PENCIL CODE

ruxuym

h̺uxuyi(mean Reynolds stress)

ruxuzm

h̺uxuzi(mean Reynolds stress)

ruyuzm

h̺uyuzi(mean Reynolds stress)

divrhourms

|∇ · (̺u)|rms

divrhoumax

|∇ · (̺u)|max

rlxm

hρyuz−zuyi

rlym

hρzux−xuzi

rlzm

hρxuy−yuxi

rlx2m

h(ρyuz−zuy)2i

rly2m

h(ρzux−xuz)2i

rlz2m

h(ρxuy−yux)2i

tot ang mom

Total angular momentum in spherical coordinates about the

axis.

dtu

δt/[cδt δx/ max |u|](time step relative to advective time step;

see §5.15)

oum

hω·ui

ou int

RVω·udV

fum

hf·ui

odel2um

hω∇2ui

o2m

hω2i ≡ h(∇ × u)2i

orms

hω2i1/2

omax

max(|ω|)

ox2m

hω2

oy2m

ω2

y

oz2m

hω2

oxuzxm

hωxuz,xi

oyuzym

hωyuz,yi

oxoym

hωxωyi

oxozm

hωxωzi

oyozm

hωyωzi

qfm

hq·fi

q2m

hq2i

qrms

hq2i1/2

qmax

max(|q|)

qom

hq·ωi

quxom

hq·(u×ω)i

pvzm

hωz+ 2Ω/̺i(z component of potential vorticity)

oumphi

hω·uiϕ

ugurmsx

(u∇u)21/2for the hydro xaver range

ugu2m

hu∇ui2

dudx

δu

δx 

Marms

hu2/c2

si(rms Mach number)

Mamax

max |u|/cs(maximum Mach number)

ekin

1

2̺u2

ekintot

2̺u2dV

uxglnrym

hux∂yln ̺i

uyglnrxm

huy∂xln ̺i

uzdivum

huz∇ · ui

uxuydivum

huxuy∇ · ui

K.3 Parameters for ‘print.in’ 191

divuHrms

(∇H·uH)rms

uxxrms

urms

x,x

uyyrms

urms

y,y

uxzrms

urms

x,z

uyzrms

urms

y,z

uzyrms

urms

z,y

dtF

δt/[cδt δx/ max |F|](time step relative to max force time step;

see §5.15) Rur(θ, φ)Ym

ℓ(θ, φ) sin(θ)dθdφ

udpxxm

components of symmetric tensor hui∂jp+uj∂ipi

Module ‘density.f90’

rhom

h̺i(mean density)

rhomxmask

h̺ifor the density xaver range

rhomzmask

h̺ifor the density zaver range

drho2m

<(̺−̺0)2>

drhom

< ̺ −̺0>

rhomin

min(ρ)

rhomax

max(ρ)

lnrhomin

min(log ρ)

lnrhomax

max(log ρ)

ugrhom

hu· ∇̺i

uglnrhom

hu· ∇ln ̺i

totmass

R̺ dV

mass

R̺ dV

vol

RdV (volume)

grhomax

max(|∇̺|)

Module ‘entropy.f90’

dtc

δt/[cδt δx/max cs](time step relative to acoustic time step;

see §5.15)

ethm

h̺ei(mean thermal [=internal] energy)

ssruzm

hs̺uz/cpi

ssuzm

hsuz/cpi

ssm

hs/cpi(mean entropy)

ss2m

h(s/cp)2i(mean squared entropy)

eem

hei

ppm

hpi

csm

hcsi

csmax

max(cs)

cgam

hcγi

pdivum

hp∇ · ui

fradbot

RFbot ·dS

fradtop

RFtop ·dS

TTtop

RTtopdS

ethtot

RV̺e dV (total thermal [=internal] energy)

dtchi

δt/[cδt,vδx2/χmax](time step relative to time step based on

heat conductivity; see §5.15)

Hmax

Hmax (net heat sources summed see §5.15)

tauhmin

Hmax (net heat sources summed see §5.15)

192 THE PENCIL CODE

dtH

δt/[cδt,scvT/Hmax](time step relative to time step based on

heat sources; see §5.15)

yHm

mean hydrogen ionization

yHmax

max of hydrogen ionization

TTm

hTi

TTmax

Tmax

TTmin

Tmin

gTmax

max(|∇T|)

ssmax

smax

ssmin

smin

gTrms

(∇T)rms

gsrms

(∇s)rms

gTxgsrms

(∇T× ∇s)rms

fconvm

hcp̺uzTi

ufpresm

h−u/ρ∇pi

Kkramersm

hKkramersi

Module ‘magnetic.f90’

eta tdep

t-dependent η

ab int

RA·BdV

jb int

Rj·BdV

b2tm

Db(t)·Rt

0b(t′)dt′E

bjtm

Db(t)·Rt

0j(t′)dt′E

jbtm

Dj(t)·Rt

0b(t′)dt′E

b2ruzm

B2ρuz

b2uzm

B2uz

ubbzm

h(u·B)Bzi

b1m

h|B|i

b2m

B2

EEM

B2/2

b4m

B4

bm2

max(B2)

j2m

j2

jm2

max(j2)

abm

hA·Bi

abumx

huxA·Bi

abumy

huyA·Bi

abumz

huzA·Bi

abmh

hA·Bi(temp)

abmn

hA·Bi(north)

abms

hA·Bi(south)

abrms

h(A·B)2i1/2

jbrms

h(j·B)2i1/2

ajm

hj·Ai

jbm

hj·Bi

jbmh

hJ·Bi(temp)

jbmn

hJ·Bi(north)

jbms

hJ·Bi(south)

K.3 Parameters for ‘print.in’ 193

ubm

hu·Bi

dubrms

h(u−B)2i1/2

dobrms

h(ω−B)2i1/2

uxbxm

huxBxi

uybxm

huyBxi

uzbxm

huzBxi

uxbym

huxByi

uybym

huyByi

uzbym

huzByi

uxbzm

huxBzi

uybzm

huyBzi

uzbzm

huzBzi

cosubm

hU·B/(|U||B|)i

jxbxm

hjxBxi

jybxm

hjyBxi

jzbxm

hjzBxi

jxbym

hjxByi

jybym

hjyByi

jzbym

hjzByi

jxbzm

hjxBzi

jybzm

hjyBzi

jzbzm

hjzBzi

uam

hu·Ai

ujm

hu·Ji

fbm

hf·Bi

fxbxm

hfxBxi

epsM

ηµ0j2

epsAD

hρ−1tAD(J×B)2i(heating by ion-neutrals friction)

bxpt

Bx(x1, y1, z1, t)

bypt

By(x1, y1, z1, t)

bzpt

Bz(x1, y1, z1, t)

jxpt

Jx(x1, y1, z1, t)

jypt

Jy(x1, y1, z1, t)

jzpt

Jz(x1, y1, z1, t)

Expt

Ex(x1, y1, z1, t)

Eypt

Ey(x1, y1, z1, t)

Ezpt

Ez(x1, y1, z1, t)

axpt

Ax(x1, y1, z1, t)

aypt

Ay(x1, y1, z1, t)

azpt

Az(x1, y1, z1, t)

bxp2

Bx(x2, y2, z2, t)

byp2

By(x2, y2, z2, t)

bzp2

Bz(x2, y2, z2, t)

jxp2

Jx(x2, y2, z2, t)

jyp2

Jy(x2, y2, z2, t)

jzp2

Jz(x2, y2, z2, t)

Exp2

Ex(x2, y2, z2, t)

Eyp2

Ey(x2, y2, z2, t)

Ezp2

Ez(x2, y2, z2, t)

axp2

Ax(x2, y2, z2, t)

194 THE PENCIL CODE

ayp2

Ay(x2, y2, z2, t)

azp2

Az(x2, y2, z2, t)

exabot

RE×AdS|bot

exatop

RE×AdS|top

emag

2µ0B2dV

brms

B21/2

bfrms

DB′2E1/2

bf2m

DB′2E

bf4m

DB′4E

bmax

max(|B|)

bxmin

min(|Bx|)

bymin

min(|By|)

bzmin

min(|Bz|)

bxmax

max(|Bx|)

bymax

max(|By|)

bzmax

max(|Bz|)

bbxmax

max(|Bx|)excludingBvext

bbymax

max(|By|)excludingBvext

bbzmax

max(|Bz|)excludingBvext

jxmax

max(|jvx|)

jymax

max(|jvy|)

jzmax

max(|jvz|)

jrms

j21/2

hjrms

j21/2

jmax

max(|j|)

vArms

B2/̺1/2

vAmax

max(B2/̺)1/2

dtb

δt/[cδt δx/vA,max](time step relative to Alfv´

en time step; see

§5.15)

dteta

δt/[cδt,vδx2/ηmax](time step relative to resistive time step;

see §5.15)

a2m

A2

arms

A21/2

amax

max(|A|)

divarms

h(∇ · A)2i1/2

beta1m

B2/(2µ0p)(mean inverse plasma beta)

beta1max

max[B2/(2µ0p)] (maximum inverse plasma beta)

betam

hβi

betamax

max β

betamin

min β

bxm

hBxi

bym

hByi

bzm

hBzi

bxbym

hBxByi

bmx

DhBi2

yzE1/2(energy of yz-averaged mean ﬁeld)

bmy

hBi2

xz1/2(energy of xz-averaged mean ﬁeld)

K.3 Parameters for ‘print.in’ 195

bmz

DhBi2

xyE1/2(energy of xy-averaged mean ﬁeld)

bmzS2

DhBSi2

xyE

bmzA2

DhBAi2

xyE

jmx

DhJi2

yzE1/2(energy of yz-averaged mean current density)

jmy

hJi2

xz1/2(energy of xz-averaged mean current density)

jmz

DhJi2

xyE1/2(energy of xy-averaged mean current density)

bmzph

Phase of a Beltrami ﬁeld

bmzphe

Error of phase of a Beltrami ﬁeld

bsinphz

sine of phase of a Beltrami ﬁeld

bcosphz

cosine of phase of a Beltrami ﬁeld

emxamz3

DhEixy × hAixyE(xy-averaged mean ﬁeld helicity ﬂux)

embmz

DhEixy · hBixyE(xy-averaged mean ﬁeld helicity production

)

ambmz

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld)

ambmzh

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, temp)

ambmzn

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, north)

ambmzs

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, south)

jmbmz

DhJixy · hBixyE(current helicity of xy-averaged mean ﬁeld)

Rmmz

D|u×B|

|ηJ|Exy

kx aa

kmz

DhJixy · hBixyE/DhBi2

xyE

bx2m

hB2

by2m

B2

y

bz2m

hB2

uxbm

hu×Bi · B0/B2

jxbm

hj×Bi · B0/B2

vmagfricmax

max(1/νmag|j×B/B2|)

vmagfricrms

1/νmag|j×B/B2|21/2

b3b21m

hB3B2,1i

b3b12m

hB3B1,2i

b1b32m

hB1B3,2i

b1b23m

hB1B2,3i

b2b13m

hB2B1,3i

b2b31m

hB2B3,1i

uxbmx

h(u×B)xi

uxbmy

h(u×B)yi

uxbmz

h(u×B)zi

jxbmx

h(j×B)xi

196 THE PENCIL CODE

jxbmy

h(j×B)yi

jxbmz

h(j×B)zi

examx

hE×Ai|x

examy

hE×Ai|y

examz

hE×Ai|z

exjmx

hE×Ji|x

exjmy

hE×Ji|y

exjmz

hE×Ji|z

dexbmx

h∇ × E×Bi|x

dexbmy

h∇ × E×Bi|y

dexbmz

h∇ × E×Bi|z

phibmx

hφBi|x

phibmy

hφBi|y

phibmz

hφBi|z

b2divum

B2∇ · u

jdel2am

hJ· ∇2A)i

ujxbm

hu·(J×B)i

jxbrmax

max(|J×B/ρ|)

jxbr2m

h(J×B/ρ)2i

bmxy rms

p[hbxiz(x, y)]2+ [hbyiz(x, y)]2+ [hbziz(x, y)]2

etasmagm

Mean of Smagorinsky resistivity

etasmagmin

Min of Smagorinsky resistivity

etasmagmax

Max of Smagorinsky resistivity

etavamax

Max of artiﬁcial resistivity η∼vA

etajmax

Max of artiﬁcial resistivity η∼J/√ρ

etaj2max

Max of artiﬁcial resistivity η∼J2/ρ

etajrhomax

Max of artiﬁcial resistivity η∼J/ρ

cosjbm

hJ·B/(|J||B|)i

jparallelm

Mean value of the component of J parallel to B

jperpm

Mean value of the component of J perpendicular to B

hjparallelm

Mean value of the component of Jhyper parallel to B

hjperpm

Mean value of the component of Jhyper perpendicular to B

brmsx

B21/2for the magnetic xaver range

brmsz

B21/2for the magnetic zaver range

Exmxy

hExiz

Eymxy

hEyiz

Ezmxy

hEziz

Module ‘pscalar.f90’

rhoccm

h̺ci

ccmax

max(c)

ccglnrm

hc∇z̺i

Module ‘1D_loop.f90’

dtchi2

heatconduction

dtrad

radiative loss from RTV

dtspitzer

Spitzer heat conduction time step

qmax

max of heat ﬂux vector

qrms

rms of heat ﬂux vector

Module ‘advective_gauge.f90’

K.3 Parameters for ‘print.in’ 197

Lamm

hΛi

Lampt

Λ(x1, y1, z1)

Lamp2

Λ(x2, y2, z2)

Lamrms

hΛ2i1/2

Lambzm

hΛBzi

Lambzmz

hΛBzixy

gLambm

hΛBi

apbrms

h(A′B)2i1/2

jxarms

h(J×A)2i1/2

jxaprms

h(J×A′)2i1/2

jxgLamrms

h(J× ∇Λ)2i1/2

gLamrms

h(∇Λ)2i1/2

divabrms

h[(∇ · A)B]2i1/2

divapbrms

h[(∇ · A′)B]2i1/2

d2Lambrms

h[(∇2Λ)B]2i1/2

d2Lamrms

h[∇2Λ]2i1/2

Module ‘anelastic.f90’

rhom

h̺i(mean density)

ugrhom

hu· ∇̺i

mass

R̺ dV

divrhoum

h∇ · (̺u)i

divrhourms

|∇ · (̺u)|rms

divrhoumax

|∇ · (̺u)|max

Module ‘bfield.f90’

bmax

max B

bmin

min B

brms

hB2i1/2

hBi

b2m

hB2i

bxmax

max |Bx|

bymax

max |By|

bzmax

max |Bz|

bxm

hBxi

bym

hByi

bzm

hBzi

bx2m

hB2

by2m

hB2

bz2m

hB2

bxbym

hBxByi

bxbzm

hBxBzi

bybzm

hByBzi

dbxmax

max |Bx−Bext,x|

dbymax

max |By−Bext,y|

dbzmax

max |Bz−Bext,z|

dbxm

hBx−Bext,xi

dbym

hBy−Bext,yi

198 THE PENCIL CODE

dbzm

hBz−Bext,zi

dbx2m

h(Bx−Bext,x)2i

dby2m

h(By−Bext,y)2i

dbz2m

h(Bz−Bext,z)2i

jmax

max J

jmin

min J

jrms

hJ2i1/2

hJi

j2m

hJ2i

jxmax

max |Jx|

jymax

max |Jy|

jzmax

max |Jz|

jxm

hJxi

jym

hJyi

jzm

hJzi

jx2m

hJ2

jy2m

hJ2

jz2m

hJ2

divbmax

max |∇ · B|

divbrms

h(∇ · B)2i1/2

betamax

max β

betamin

min β

betam

hβi

vAmax

max vA

vAmin

min vA

vAm

hvAi

Module ‘chemistry.f90’

dtchem

Module ‘chemistry_simple.f90’

dtchem

Module ‘chiral_mhd.f90’

muSm

hµSi

muSrms

hµ2

Si1/2

mu5m

hµ5i

mu5rms

hµ2

5i1/2

gmu5rms

h(∇µ5)2i1/2

gmu5mx

h∇µ5ix

gmu5my

h∇µ5iy

gmu5mz

h∇µ5iz

bgmu5rms

h(B· ∇µ5)2i1/2

bgmuSrms

h(B· ∇µS)2i1/2

mu5bjm

hµ5((∇ × B)·B)i

mu5bjrms

h(µ5((∇ × B)·B))2i1/2

dt mu5 1

min(µ5/B2)δx/(λη)

dt mu5 2

(ληmin(B2))−1

dt mu5 3

δx2/D5

K.3 Parameters for ‘print.in’ 199

dt mu5 4

δx2/D5

dt muS 1

min(µ5/B2)δx/(λη)

dt muS 2

(ληmin(B2))−1

dt bb 1

δx/(ηmax(µ5))

dt chiral

total time-step contribution from chiral MHD

mu5bxm

hµ5Bxi

mu5b2m

hµ5B2i

jxm

hJxi

Module ‘coronae.f90’

dtchi2

δt/[cδt,vδx2/χmax](time step relative to time step based on

heat conductivity; see §5.15)

dtspitzer

Spitzer heat conduction time step

dtrad

radiative loss from RTV

Module ‘cosmicray_current.f90’

ekincr

1

2̺u2

cr

ethmcr

h̺crecri

Module ‘density_stratified.f90’

mass

Rρ d3x

rhomin

min |ρ|

rhomax

max |ρ|

drhom

h∆ρ/ρ0i

drho2m

h(∆ρ/ρ0)2i

drhorms

h∆ρ/ρ0irms

drhomax

max |∆ρ/ρ0|

Module ‘detonate.f90’

detn

Number of detonated sites (summed over time steps between

adjacent outputs)

dettot

Total energy input (summed over time steps between adjacent

outputs)

Module ‘dustdensity.f90’

KKm

PTcoag

KK2m

PTcoag

MMxm

PMx

k,coag

MMym

PMy

k,coag

MMzm

PMz

k,coag

Module ‘entropy_anelastic.f90’

dtc

δt/[cδt δx/max cs](time step relative to acoustic time step;

see §5.15)

ethm

h̺ei(mean thermal [=internal] energy)

ssm

hs/cpi(mean entropy)

ss2m

h(s/cp)2i(mean squared entropy)

eem

hei

ppm

hpi

csm

hcsi

pdivum

hp∇ui

200 THE PENCIL CODE

fradbot

RFbot ·dS

fradtop

RFtop ·dS

TTtop

RTtopdS

ethtot

RV̺e dV (total thermal [=internal] energy)

dtchi

δt/[cδt,vδx2/χmax](time step relative to time step based on

heat conductivity; see §5.15)

ssmxy

hsiz

ssmxz

hsiy

Module ‘gravitational_waves.f90’

hhT2m

hh2

hhX2m

hh2

hhThhXm

hhThXi

ggTpt

gT(x1, y1, z1, t)

strTpt

ST(x1, y1, z1, t)

strXpt

SX(x1, y1, z1, t)

Module ‘gravitational_waves_hTXk.f90’

g11pt

g11(x1, y1, z1, t)

g22pt

g22(x1, y1, z1, t)

g33pt

g33(x1, y1, z1, t)

g12pt

g12(x1, y1, z1, t)

g23pt

g23(x1, y1, z1, t)

g31pt

g31(x1, y1, z1, t)

hhTpt

hT(x1, y1, z1, t)

hhXpt

hX(x1, y1, z1, t)

ggTpt

hT(x1, y1, z1, t)

ggXpt

hX(x1, y1, z1, t)

hhTp2

hT(x1, y1, z1, t)

hhXp2

hX(x1, y1, z1, t)

ggTp2

hT(x1, y1, z1, t)

ggXp2

hX(x1, y1, z1, t)

hrms

hh2

T+h2

Xi1/2

EEGW

hg2

T+g2

Xic2/(32πG)

gg2m

hg2

T+g2

hhT2m

hh2

hhX2m

hh2

hhTXm

hhThXi

ggT2m

hg2

ggX2m

hg2

ggTXm

hgTgXi

Module ‘gravitational_waves_hij6.f90’

h22rms

hrms

h33rms

hrms

h23rms

hrms

g11pt

g11(x1, y1, z1, t)

g22pt

g22(x1, y1, z1, t)

g33pt

g33(x1, y1, z1, t)

g12pt

g12(x1, y1, z1, t)

K.3 Parameters for ‘print.in’ 201

g23pt

g23(x1, y1, z1, t)

g31pt

g31(x1, y1, z1, t)

hhTpt

hT(x1, y1, z1, t)

hhXpt

hX(x1, y1, z1, t)

ggTpt

hT(x1, y1, z1, t)

ggXpt

hX(x1, y1, z1, t)

hhTp2

hT(x1, y1, z1, t)

hhXp2

hX(x1, y1, z1, t)

ggTp2

hT(x1, y1, z1, t)

ggXp2

hX(x1, y1, z1, t)

hrms

hh2

T+h2

Xi1/2

EEGW

hg2

T+g2

Xic2/(32πG)

gg2m

hg2

T+g2

hhT2m

hh2

hhX2m

hh2

hhTXm

hhThXi

ggT2m

hg2

ggX2m

hg2

ggTXm

hgTgXi

ggTm

hgTi

ggXm

hgXi

hijij2m

hh2

ij,iji

gijij2m

hg2

ij,iji

Module ‘gravity_simple.f90’

epot

h̺Φgravi(mean potential energy)

epottot

RV̺ΦgravdV (total potential energy)

ugm

hu·gi

Module ‘heatflux.f90’

dtspitzer

Spitzer heat conduction time step

dtq

heatﬂux time step

dtq2

heatﬂux time step due to tau

qmax

max(|q|)

tauqmax

max(|τSpitzer|)

qxmin

min(|qx|)

qymin

min(|qy|)

qzmin

min(|qz|)

qxmax

max(|qx|)

qymax

max(|qy|)

qzmax

max(|qz|)

qrms

p(|q|2)

qsatmin

minimum of qsat/qabs

qsatrms

rms of qsat/abs

Module ‘lorenz_gauge.f90’

phim

hφi

phipt

φ(x1, y1, z1)

phip2

φ(x2, y2, z2)

phibzm

hφBzi

202 THE PENCIL CODE

phibzmz

hφBzixy

Module ‘magnetic_shearboxJ.f90’

ab int

RA·BdV

jb int

Rj·BdV

b2tm

Db(t)·Rt

0b(t′)dt′E

bjtm

Db(t)·Rt

0j(t′)dt′E

jbtm

Dj(t)·Rt

0b(t′)dt′E

b2ruzm

B2ρuz

b2uzm

B2uz

ubbzm

h(u·B)Bzi

b1m

h|B|i

b2m

B2

bm2

max(B2)

j2m

j2

jm2

max(j2)

abm

hA·Bi

abumx

huxA·Bi

abumy

huyA·Bi

abumz

huzA·Bi

abmh

hA·Bi(temp)

abmn

hA·Bi(north)

abms

hA·Bi(south)

abrms

h(A·B)2i1/2

jbrms

h(j·B)2i1/2

ajm

hj·Ai

jbm

hj·Bi

jbmh

hJ·Bi(temp)

jbmn

hJ·Bi(north)

jbms

hJ·Bi(south)

ubm

hu·Bi

dubrms

h(u−B)2i1/2

dobrms

h(ω−B)2i1/2

uxbxm

huxBxi

uybxm

huyBxi

uzbxm

huzBxi

uxbym

huxByi

uybym

huyByi

uzbym

huzByi

uxbzm

huxBzi

uybzm

huyBzi

uzbzm

huzBzi

cosubm

hU·B/(|U||B|)i

jxbxm

hjxBxi

jybxm

hjyBxi

jzbxm

hjzBxi

jxbym

hjxByi

jybym

hjyByi

K.3 Parameters for ‘print.in’ 203

jzbym

hjzByi

jxbzm

hjxBzi

jybzm

hjyBzi

jzbzm

hjzBzi

uam

hu·Ai

ujm

hu·Ji

fbm

hf·Bi

fxbxm

hfxBxi

epsM

ηµ0j2

epsAD

hρ−1tAD(J×B)2i(heating by ion-neutrals friction)

bxpt

Bx(x1, y1, z1, t)

bypt

By(x1, y1, z1, t)

bzpt

Bz(x1, y1, z1, t)

jxpt

Jx(x1, y1, z1, t)

jypt

Jy(x1, y1, z1, t)

jzpt

Jz(x1, y1, z1, t)

Expt

Ex(x1, y1, z1, t)

Eypt

Ey(x1, y1, z1, t)

Ezpt

Ez(x1, y1, z1, t)

axpt

Ax(x1, y1, z1, t)

aypt

Ay(x1, y1, z1, t)

azpt

Az(x1, y1, z1, t)

bxp2

Bx(x2, y2, z2, t)

byp2

By(x2, y2, z2, t)

bzp2

Bz(x2, y2, z2, t)

jxp2

Jx(x2, y2, z2, t)

jyp2

Jy(x2, y2, z2, t)

jzp2

Jz(x2, y2, z2, t)

Exp2

Ex(x2, y2, z2, t)

Eyp2

Ey(x2, y2, z2, t)

Ezp2

Ez(x2, y2, z2, t)

axp2

Ax(x2, y2, z2, t)

ayp2

Ay(x2, y2, z2, t)

azp2

Az(x2, y2, z2, t)

exabot

RE×AdS|bot

exatop

RE×AdS|top

emag

2µ0B2dV

brms

B21/2

bfrms

DB′2E1/2

bmax

max(|B|)

bxmin

min(|Bx|)

bymin

min(|By|)

bzmin

min(|Bz|)

bxmax

max(|Bx|)

bymax

max(|By|)

bzmax

max(|Bz|)

bbxmax

max(|Bx|)excludingBvext

bbymax

max(|By|)excludingBvext

bbzmax

max(|Bz|)excludingBvext

204 THE PENCIL CODE

jxmax

max(|jvx|)

jymax

max(|jvy|)

jzmax

max(|jvz|)

jrms

j21/2

hjrms

j21/2

jmax

max(|j|)

vArms

B2/̺1/2

vAmax

max(B2/̺)1/2

dtb

δt/[cδt δx/vA,max](time step relative to Alfv´

en time step; see

§5.15)

dteta

δt/[cδt,vδx2/ηmax](time step relative to resistive time step;

see §5.15)

a2m

A2

arms

A21/2

amax

max(|A|)

divarms

h(∇ · A)2i1/2

beta1m

B2/(2µ0p)(mean inverse plasma beta)

beta1max

max[B2/(2µ0p)] (maximum inverse plasma beta)

betam

hβi

betamax

max β

betamin

min β

bxm

hBxi

bym

hByi

bzm

hBzi

bxbym

hBxByi

bmx

DhBi2

yzE1/2(energy of yz-averaged mean ﬁeld)

bmy

hBi2

xz1/2(energy of xz-averaged mean ﬁeld)

bmz

DhBi2

xyE1/2(energy of xy-averaged mean ﬁeld)

bmzS2

DhBSi2

xyE

bmzA2

DhBAi2

xyE

jmx

DhJi2

yzE1/2(energy of yz-averaged mean current density)

jmy

hJi2

xz1/2(energy of xz-averaged mean current density)

jmz

DhJi2

xyE1/2(energy of xy-averaged mean current density)

bmzph

Phase of a Beltrami ﬁeld

bmzphe

Error of phase of a Beltrami ﬁeld

bsinphz

sine of phase of a Beltrami ﬁeld

bcosphz

cosine of phase of a Beltrami ﬁeld

emxamz3

DhEixy × hAixyE(xy-averaged mean ﬁeld helicity ﬂux)

embmz

DhEixy · hBixyE(xy-averaged mean ﬁeld helicity production

)

ambmz

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld)

K.3 Parameters for ‘print.in’ 205

ambmzh

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, temp)

ambmzn

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, north)

ambmzs

DhAixy · hBixyE(magnetic helicity of xy-averaged mean

ﬁeld, south)

jmbmz

DhJixy · hBixyE(current helicity of xy-averaged mean ﬁeld)

kx aa

kmz

DhJixy · hBixyE/DhBi2

xyE

bx2m

hB2

by2m

B2

y

bz2m

hB2

uxbm

hu×Bi · B0/B2

jxbm

hj×Bi · B0/B2

magfricmax

Magneto-Frictional velocity hj×Bi · B2

b3b21m

hB3B2,1i

b3b12m

hB3B1,2i

b1b32m

hB1B3,2i

b1b23m

hB1B2,3i

b2b13m

hB2B1,3i

b2b31m

hB2B3,1i

uxbmx

h(u×B)xi

uxbmy

h(u×B)yi

uxbmz

h(u×B)zi

jxbmx

h(j×B)xi

jxbmy

h(j×B)yi

jxbmz

h(j×B)zi

examx

hE×Ai|x

examy

hE×Ai|y

examz

hE×Ai|z

exjmx

hE×Ji|x

exjmy

hE×Ji|y

exjmz

hE×Ji|z

dexbmx

h∇ × E×Bi|x

dexbmy

h∇ × E×Bi|y

dexbmz

h∇ × E×Bi|z

phibmx

hφBi|x

phibmy

hφBi|y

phibmz

hφBi|z

b2divum

B2∇ · u

ujxbm

hu·(J×B)i

jxbrmax

max(|J×B/ρ|)

jxbr2m

h(J×B/ρ)2i

bmxy rms

p[hbxiz(x, y)]2+ [hbyiz(x, y)]2+ [hbziz(x, y)]2

etasmagm

Mean of Smagorinsky resistivity

etasmagmin

Min of Smagorinsky resistivity

etasmagmax

Max of Smagorinsky resistivity

etavamax

Max of artiﬁcial resistivity η∼vA

206 THE PENCIL CODE

etajmax

Max of artiﬁcial resistivity η∼J/√ρ

etaj2max

Max of artiﬁcial resistivity η∼J2/ρ

etajrhomax

Max of artiﬁcial resistivity η∼J/ρ

cosjbm

hJ·B/(|J||B|)i

jparallelm

Mean value of the component of J parallel to B

jperpm

Mean value of the component of J perpendicular to B

hjparallelm

Mean value of the component of Jhyper parallel to B

hjperpm

Mean value of the component of Jhyper perpendicular to B

brmsx

B21/2for the magnetic xaver range

brmsz

B21/2for the magnetic zaver range

Exmxy

hExiz

Eymxy

hEyiz

Ezmxy

hEziz

Module ‘meanfield.f90’

qsm

qp(B)

qpm

qp(B)

qem

qe(B), in the paper referred to as qg(B)

qam

qa(B)

alpm

hαi

etatm

hηti

EMFmz1

hEixy |x

EMFmz2

hEixy |y

EMFmz3

hEixy |z

EMFdotBm

hE · Bi

EMFdotB int

RE · BdV

Module ‘meanfield_demfdt.f90’

EMFrms

(hEi)rms

EMFmax

max(hEi)

EMFmin

min(hEi)

Module ‘noentropy.f90’

dtc

δt/[cδt δx/max cs](time step relative to acoustic time step;

see §5.15)

ethm

h̺ei(mean thermal [=internal] energy)

pdivum

hp∇ui

Module ‘particles_caustics.f90’

TrSigmapm

hTr [σ]i

blowupm

Mean no. of times σfalls below cutoff

lnVpm

Mean of (logarithm of) Volume around an inertial particle

Module ‘particles_chemistry.f90’

Shchm

meanparticleSherwoodnumber

Module ‘particles_dust.f90’

xpm

xpart

xpmin

xpart

xpmax

xpart

K.3 Parameters for ‘print.in’ 207

xp2m

part

vrelpabsm

Absolutevalueofmeanrelativevelocity

vpxm

upart

vpx2m

part

ekinp

Ekin,part

vpxmax

MAX(upart)

vpxmin

MIN(upart)

npm

meanparticlenumberdensity

Module ‘particles_dust_brdeplete.f90’

xpm

xpart

xp2m

part

vrelpabsm

Absolutevalueofmeanrelativevelocity

vpxm

upart

vpx2m

part

ekinp

Ekin,part

vpxmax

MAX(upart)

vpxmin

MIN(upart)

npm

meanparticlenumberdensity

Module ‘particles_lagrangian.f90’

xpm

xpart

xp2m

part

vrelpabsm

Absolutevalueofmeanrelativevelocity

vpxm

upart

vpx2m

part

ekinp

Ekin,part

vpxmax

MAX(upart)

vpxmin

MIN(upart)

npm

meanparticlenumberdensity

Module ‘particles_mass_swarm.f90’

mpm

mpmin

minjmp,j

mpmax

maxjmp,j

Module ‘particles_surfspec.f90’

dtpchem

dtparticle,chemistry

Module ‘polymer.f90’

polytrm

hT r[Cij]i

frmax

max(f(r))

Module ‘r75612.f90’

h22rms

hrms

h33rms

hrms

h23rms

hrms

g11pt

g11(x1, y1, z1, t)

g22pt

g22(x1, y1, z1, t)

g33pt

g33(x1, y1, z1, t)

g12pt

g12(x1, y1, z1, t)

208 THE PENCIL CODE

g23pt

g23(x1, y1, z1, t)

g31pt

g31(x1, y1, z1, t)

hhTpt

hT(x1, y1, z1, t)

hhXpt

hX(x1, y1, z1, t)

ggTpt

hT(x1, y1, z1, t)

ggXpt

hX(x1, y1, z1, t)

hhTp2

hT(x1, y1, z1, t)

hhXp2

hX(x1, y1, z1, t)

ggTp2

hT(x1, y1, z1, t)

ggXp2

hX(x1, y1, z1, t)

hrms

hh2

T+h2

Xi1/2

gg2m

hg2

T+g2

hhT2m

hh2

hhX2m

hh2

hhTXm

hhThXi

ggT2m

hg2

ggX2m

hg2

ggTXm

hgTgXi

ggTm

hgTi

ggXm

hgXi

Module ‘r75759.f90’

h22rms

hrms

h33rms

hrms

h23rms

hrms

g11pt

g11(x1, y1, z1, t)

g22pt

g22(x1, y1, z1, t)

g33pt

g33(x1, y1, z1, t)

g12pt

g12(x1, y1, z1, t)

g23pt

g23(x1, y1, z1, t)

g31pt

g31(x1, y1, z1, t)

hhTpt

hT(x1, y1, z1, t)

hhXpt

hX(x1, y1, z1, t)

ggTpt

hT(x1, y1, z1, t)

ggXpt

hX(x1, y1, z1, t)

hhTp2

hT(x1, y1, z1, t)

hhXp2

hX(x1, y1, z1, t)

ggTp2

hT(x1, y1, z1, t)

ggXp2

hX(x1, y1, z1, t)

hrms

hh2

T+h2

Xi1/2

gg2m

hg2

T+g2

hhT2m

hh2

hhX2m

hh2

hhTXm

hhThXi

ggT2m

hg2

ggX2m

hg2

ggTXm

hgTgXi

ggTm

hgTi

ggXm

hgXi

K.3 Parameters for ‘print.in’ 209

Module ‘shear.f90’

dtshear

advec shear/cdt

deltay

Module ‘shock.f90’

shockmax

Max shock number

Module ‘shock_highorder.f90’

gshockmax

max |∇νshock|

Module ‘solar_corona.f90’

dtvel

Velocity driver time step

dtnewt

Radiative cooling time step

dtradloss

Radiative losses time step

dtchi2

δt/[cδt,vδx2/χmax](time step relative to time step based on

heat conductivity; see §5.15)

dtspitzer

Spitzer heat conduction time step

mag ﬂux

Total vertical magnetic ﬂux at

Module ‘solid_cells_CGEO.f90’

Module ‘solid_cells_ogrid_chemistry.f90’

dtchem

Module ‘solid_cells_reactive.f90’

Module ‘temperature_idealgas.f90’

TTmax

max(T)

gTmax

max(|∇T|)

TTmin

min(T)

TTm

hTi

TTzmask

hTifor the temp zaver range

TT2m

hT2i

TugTm

hTu· ∇Ti

Trms

phT2i

uxTm

huxTi

uyTm

huyTi

uzTm

huzTi

gT2m

h(∇T)2i

guxgTm

h∇ux· ∇Ti

guygTm

h∇uy· ∇Ti

guzgTm

h∇uz· ∇Ti

Tugux uxugTm

hTu· ∇ux+uxu· ∇Ti=hu· ∇(uxT)i

Tuguy uyugTm

hTu· ∇uy+uyu· ∇Ti=hu· ∇(uyT)i

Tuguz uzugTm

hTu· ∇uz+uzu· ∇Ti=hu· ∇(uzT)i

Tdxpm

hT dp/dxi

Tdypm

hT dp/dyi

Tdzpm

hT dp/dzi

fradtop

<−KdT

dz >top (top radiative ﬂux)

fradbot

<−KdT

dz >bot (bottom radiative ﬂux)

yHmax

DOCUMENT ME

210 THE PENCIL CODE

yHmin

DOCUMENT ME

yHm

DOCUMENT ME

ethm

hethi=hcvρT i(mean thermal energy)

eem

hei=hcvTi(mean internal energy)

ethtot

RV̺e dV (total thermal energy)

ssm

thcool

τcool

ppm

csm

csmax

max(cs)

dtc

δt/[cδt δx/max cs](time step relative to acoustic time step;

see §5.15)

dtchi

δt/[cδt,vδx2/χmax](time step relative to time step based on

heat conductivity; see §5.15)

Emzmask

hn2exp −(log T−log T0)2/(δlog T)2ithe emiss zaver range

Module ‘temperature_ionization.f90’

TTmax

max(T)

TTmin

min(T)

TTm

hTi

ethm

hethi=hcvρT i(mean thermal energy)

eem

hei(mean internal energy)

ppm

hpi

Module ‘test_chemistry.f90’

dtchem

Module ‘testfield_axisym.f90’

alpPERP

α⊥

alpPARA

α⊥

gam

betPERP

β⊥

betPARA

β⊥

del

kapPERP

κ⊥

kapPARA

κ⊥

alpPERPz

α⊥(z)

alpPARAz

α⊥(z)

gamz

γ(z)

betPERPz

β⊥(z)

betPARAz

β⊥(z)

delz

δ(z)

kapPERPz

κ⊥(z)

kapPARAz

κ⊥(z)

muz

µ(z)

bx1pt

bx2pt

bx3pt

b1rms

hb2

1i1/2

K.3 Parameters for ‘print.in’ 211

b2rms

hb2

2i1/2

b3rms

hb2

3i1/2

Module ‘testfield_axisym2.f90’

alpPERP

α⊥

alpPARA

α⊥

gam

betPERP

β⊥

betPARA

β⊥

del

kapPERP

κ⊥

kapPARA

κ⊥

bx1pt

bx2pt

bx3pt

b1rms

hb2

1i1/2

b2rms

hb2

2i1/2

b3rms

hb2

3i1/2

Module ‘testfield_axisym4.f90’

alpPERP

α⊥

alpPARA

α⊥

gam

betPERP

β⊥

betPERP2

β(2)

⊥

betPARA

β⊥

del

del2

δ(2)

kapPERP

κ⊥

kapPERP2

κ(2)

⊥

kapPARA

κ⊥

mu2

µ(2)

alpPERPz

α⊥(z)

alpPARAz

α⊥(z)

gamz

γ(z)

betPERPz

β⊥(z)

betPARAz

β⊥(z)

delz

δ(z)

kapPERPz

κ⊥(z)

kapPARAz

κ⊥(z)

muz

µ(z)

bx1pt

bx2pt

bx3pt

b1rms

hb2

1i1/2

b2rms

hb2

2i1/2

b3rms

hb2

3i1/2

212 THE PENCIL CODE

Module ‘testfield_compress_z.f90’

alp11

α11

alp21

α21

alp31

α31

alp12

α12

alp22

α22

alp32

α32

eta11

η11k

eta21

η21k

eta12

η12k

eta22

η22k

alpK

αK

alpM

αM

alpMK

αMK

phi11

φ11

phi21

φ21

phi12

φ12

phi22

φ22

phi32

φ32

psi11

ψ11k

psi21

ψ21k

psi12

ψ12k

psi22

ψ22k

phiK

φK

phiM

φM

phiMK

φMK

alp11cc

α11 cos2kz

alp21sc

α21 sin kz cos kz

alp12cs

α12 cos kz sin kz

alp22ss

α22 sin2kz

eta11cc

η11 cos2kz

eta21sc

η21 sin kz cos kz

eta12cs

η12 cos kz sin kz

eta22ss

η22 sin2kz

s2kzDFm

hsin 2kz∇ · Fi

M11

M22

M33

M11cc

M11 cos2kz

M11ss

M11 sin2kz

M22cc

M22 cos2kz

M22ss

M22 sin2kz

M12cs

M12 cos kz sin kz

bx11pt

b11

bx21pt

b21

bx12pt

b12

bx22pt

b22

bx0pt

by11pt

b11

by21pt

b21

K.3 Parameters for ‘print.in’ 213

by12pt

b12

by22pt

b22

by0pt

u11rms

hu2

11i1/2

u21rms

hu2

21i1/2

u12rms

hu2

12i1/2

u22rms

hu2

22i1/2

j11rms

hj2

11i1/2

b11rms

hb2

11i1/2

b21rms

hb2

21i1/2

b12rms

hb2

12i1/2

b22rms

hb2

22i1/2

ux0m

hu0xi

uy0m

u0y

ux11m

hu11xi

uy11m

u11y

u0rms

hu2

0i1/2

b0rms

hb2

0i1/2

jb0m

hjb0i

E11rms

hE2

11i1/2

E21rms

hE2

21i1/2

E12rms

hE2

12i1/2

E22rms

hE2

22i1/2

E0rms

hE2

0i1/2

Ex11pt

E11

Ex21pt

E21

Ex12pt

E12

Ex22pt

E22

Ex0pt

Ey11pt

E11

Ey21pt

E21

Ey12pt

E12

Ey22pt

E22

Ey0pt

bamp

E111z

E11

E211z

E11

E311z

E11

E121z

E21

E221z

E21

E321z

E21

E112z

E12

E212z

E12

E312z

E12

E122z

E22

E222z

E22

E322z

E22

E10z

214 THE PENCIL CODE

E20z

E30z

EBpq

E · Bpq

E0Um

E0·U

E0Wm

E0·W

bx0mz

hbxixy

by0mz

hbyixy

bz0mz

hbzixy

M11z

hM11ixy

M22z

hM22ixy

M33z

hM33ixy

Module ‘testfield_meri.f90’

E11xy

E12xy

E13xy

E21xy

E22xy

E23xy

E31xy

E32xy

E33xy

E41xy

E42xy

E43xy

E51xy

E52xy

E53xy

E61xy

E62xy

E63xy

E71xy

E72xy

E73xy

E81xy

E81

E82xy

E82

E83xy

E83

E91xy

E91

E92xy

E92

E93xy

E93

a11xy

α11

a12xy

α12

a13xy

α13

a21xy

α21

a22xy

α22

a23xy

α23

a31xy

α31

a32xy

α32

a33xy

α33

b111xy

¯111

K.3 Parameters for ‘print.in’ 215

b121xy

¯121

b131xy

¯131

b211xy

¯211

b221xy

¯221

b231xy

¯231

b311xy

¯311

b321xy

¯321

b331xy

¯331

b112xy

¯112

b122xy

¯122

b132xy

¯132

b212xy

¯212

b222xy

¯222

b232xy

¯232

b312xy

¯312

b322xy

¯322

b332xy

¯332

Module ‘testfield_nonlin_z.f90’

alp11

α11

alp21

α21

alp31

α31

alp12

α12

alp22

α22

alp32

α32

eta11

η11k

eta21

η21k

eta12

η12k

eta22

η22k

alpK

αK

alpM

αM

alpMK

αMK

phi11

φ11

phi21

φ21

phi12

φ12

phi22

φ22

phi32

φ32

psi11

ψ11k

psi21

ψ21k

psi12

ψ12k

psi22

ψ22k

phiK

φK

phiM

φM

phiMK

φMK

alp11cc

α11 cos2kz

alp21sc

α21 sin kz cos kz

alp12cs

α12 cos kz sin kz

alp22ss

α22 sin2kz

eta11cc

η11 cos2kz

eta21sc

η21 sin kz cos kz

216 THE PENCIL CODE

eta12cs

η12 cos kz sin kz

eta22ss

η22 sin2kz

s2kzDFm

hsin 2kz∇ · Fi

M11

M22

M33

M11cc

M11 cos2kz

M11ss

M11 sin2kz

M22cc

M22 cos2kz

M22ss

M22 sin2kz

M12cs

M12 cos kz sin kz

bx11pt

b11

bx21pt

b21

bx12pt

b12

bx22pt

b22

bx0pt

by11pt

b11

by21pt

b21

by12pt

b12

by22pt

b22

by0pt

u11rms

hu2

11i1/2

u21rms

hu2

21i1/2

u12rms

hu2

12i1/2

u22rms

hu2

22i1/2

j11rms

hj2

11i1/2

b11rms

hb2

11i1/2

b21rms

hb2

21i1/2

b12rms

hb2

12i1/2

b22rms

hb2

22i1/2

ux0m

hu0xi

uy0m

u0y

ux11m

hu11xi

uy11m

u11y

u0rms

hu2

0i1/2

b0rms

hb2

0i1/2

jb0m

hjb0i

E11rms

hE2

11i1/2

E21rms

hE2

21i1/2

E12rms

hE2

12i1/2

E22rms

hE2

22i1/2

E0rms

hE2

0i1/2

Ex11pt

E11

Ex21pt

E21

Ex12pt

E12

Ex22pt

E22

Ex0pt

Ey11pt

E11

K.3 Parameters for ‘print.in’ 217

Ey21pt

E21

Ey12pt

E12

Ey22pt

E22

Ey0pt

bamp

E111z

E11

E211z

E11

E311z

E11

E121z

E21

E221z

E21

E321z

E21

E112z

E12

E212z

E12

E312z

E12

E122z

E22

E222z

E22

E322z

E22

E10z

E20z

E30z

EBpq

E · Bpq

E0Um

E0·U

E0Wm

E0·W

bx0mz

hbxixy

by0mz

hbyixy

bz0mz

hbzixy

M11z

hM11ixy

M22z

hM22ixy

M33z

hM33ixy

Module ‘testfield_x.f90’

alp11

α11

alp21

α21

alp31

α31

alp12

α12

alp22

α22

alp32

α32

eta11

η11k

eta21

η21k

eta12

η12k

eta22

η22k

alp11cc

α11 cos2kx

alp21sc

α21 sin kx cos kx

alp12cs

α12 cos kx sin kx

alp22ss

α22 sin2kx

eta11cc

η11 cos2kx

eta21sc

η21 sin kx cos kx

eta12cs

η12 cos kx sin kx

eta22ss

η22 sin2kx

alp11 x

α11x

218 THE PENCIL CODE

alp21 x

α21x

alp12 x

α12x

alp22 x

α22x

eta11 x

η11kx

eta21 x

η21kx

eta12 x

η12kx

eta22 x

η22kx

alp11 x2

α11x2

alp21 x2

α21x2

alp12 x2

α12x2

alp22 x2

α22x2

eta11 x2

η11kx2

eta21 x2

η21kx2

eta12 x2

η12kx2

eta22 x2

η22kx2

b11rms

hb2

11i1/2

b21rms

hb2

21i1/2

b12rms

hb2

12i1/2

b22rms

hb2

22i1/2

b0rms

hb2

0i1/2

E11rms

hE2

11i1/2

E21rms

hE2

21i1/2

E12rms

hE2

12i1/2

E22rms

hE2

22i1/2

E0rms

hE2

0i1/2

E111z

E11

E211z

E11

E311z

E11

E121z

E21

E221z

E21

E321z

E21

E112z

E12

E212z

E12

E312z

E12

E122z

E22

E222z

E22

E322z

E22

E10z

E20z

E30z

EBpq

E · Bpq

bx0mz

hbxixy

by0mz

hbyixy

bz0mz

hbzixy

alp11x

α11(x, t)

alp21x

α21(x, t)

alp12x

α12(x, t)

alp22x

α22(x, t)

K.3 Parameters for ‘print.in’ 219

eta11x

η11(x, t)

eta21x

η21(x, t)

eta12x

η12(x, t)

eta22x

η22(x, t)

Module ‘testfield_xz.f90’

E111z

E11

E211z

E11

E311z

E11

E121z

E21

E221z

E21

E321z

E21

alp11

α11

alp21

α21

eta11

η113k

eta21

η213k

b11rms

hb2

11i

b21rms

hb2

21i

Module ‘testfield_z.f90’

alp11

α11

alp21

α21

alp31

α31

alp12

α12

alp22

α22

alp32

α32

alp13

α13

alp23

α23

eta11

η113kor η11kif leta rank2=T

eta21

η213kor η21kif leta rank2=T

eta31

η313k

eta12

η123kor η12kif leta rank2=T

eta22

η223kor η22kif leta rank2=T

eta32

η323k

alp11cc

α11 cos2kz

alp21sc

α21 sin kz cos kz

alp12cs

α12 cos kz sin kz

alp22ss

α22 sin2kz

eta11cc

η11 cos2kz

eta21sc

η21 sin kz cos kz

eta12cs

η12 cos kz sin kz

eta22ss

η22 sin2kz

s2kzDFm

hsin 2kz∇ · Fi

M11

M22

M33

M11cc

M11 cos2kz

M11ss

M11 sin2kz

M22cc

M22 cos2kz

M22ss

M22 sin2kz

220 THE PENCIL CODE

M12cs

M12 cos kz sin kz

bx11pt

b11

bx21pt

b21

bx12pt

b12

bx22pt

b22

bx0pt

by11pt

b11

by21pt

b21

by12pt

b12

by22pt

b22

by0pt

b11rms

hb2

11i1/2

b21rms

hb2

21i1/2

b12rms

hb2

12i1/2

b22rms

hb2

22i1/2

b0rms

hb2

0i1/2

jb0m

hjb0i

E11rms

hE2

11i1/2

E21rms

hE2

21i1/2

E12rms

hE2

12i1/2

E22rms

hE2

22i1/2

E0rms

hE2

0i1/2

Ex11pt

E11

Ex21pt

E21

Ex12pt

E12

Ex22pt

E22

Ex0pt

Ey11pt

E11

Ey21pt

E21

Ey12pt

E12

Ey22pt

E22

Ey0pt

bamp

alp11z

α11(z, t)

alp21z

α21(z, t)

alp12z

α12(z, t)

alp22z

α22(z, t)

alp13z

α13(z, t)

alp23z

α23(z, t)

eta11z

η11(z, t)

eta21z

η21(z, t)

eta12z

η12(z, t)

eta22z

η22(z, t)

uzjx1z

uzj11

uzjy1z

uzj11

uzjz1z

uzj11

uzjx2z

uzj21

uzjy2z

uzj21

K.3 Parameters for ‘print.in’ 221

uzjz2z

uzj21

uzjx3z

uzj12

uzjy3z

uzj12

uzjz3z

uzj12

uzjx4z

uzj22

uzjy4z

uzj22

uzjz4z

uzj22

E111z

E11

E211z

E11

E311z

E11

E121z

E21

E221z

E21

E321z

E21

E112z

E12

E212z

E12

E312z

E12

E122z

E22

E222z

E22

E322z

E22

E10z

E20z

E30z

EBpq

E · Bpq

E0Um

E0·U

E0Wm

E0·W

bx0mz

hbxixy

by0mz

hbyixy

bz0mz

hbzixy

M11z

hM11ixy

M22z

hM22ixy

M33z

hM33ixy

Module ‘testflow_z.f90’

gal

GAL-coefﬁcients, couple Fand U

aklam

AKA-λ-tensor, couples Fand W=∇ × U

gamma

γ-vector, couples Fand ∇ · U

ν-tensor, couples Fand ∂2U/∂z2

zeta

ζ-vector, couples Fand Gz=∇zH

ξ-vector, couples Fand ∂2H/∂z2

aklamQ

aklamQ-vector, couples Qand W

gammaQ

γQ-scalar, couples Qand ∇ · U=dUz/dz

nuQ

νQ-vector, couples Qand ∂2U/∂z2

zetaQ

ζQ-scalar, couples Qand Gz

xiQ

ξQ-scalar, couples Qand ∂2H/∂z2

αK,ij γiνij ζiξiνQ

iaklamQ

iFpq

iQpq upq2hpq2

ux0mz

huxixy

uy0mz

huyixy

uz0mz

huzixy

Module ‘testperturb.f90’

222 THE PENCIL CODE

alp11

α11

alp21

α21

alp31

α31

alp12

α12

alp22

α22

alp32

α32

eta11

η113k

eta21

η213k

eta31

η313k

eta12

η123k

eta22

η223k

eta32

η323k

Module ‘testscalar.f90’

gam11

γ(1)

gam12

γ(1)

gam13

γ(1)

gam21

γ(2)

gam22

γ(2)

gam23

γ(2)

gam31

γ(3)

gam32

γ(3)

gam33

γ(3)

kap11

κ11

kap21

κ21

kap31

κ31

kap12

κ12

kap22

κ22

kap32

κ32

kap13

κ13

kap23

κ23

kap33

κ33

gam11z

γ(1)

1(z, t)

gam12z

γ(1)

2(z, t)

gam13z

γ(1)

3(z, t)

gam21z

γ(2)

1(z, t)

gam22z

γ(2)

2(z, t)

gam23z

γ(2)

3(z, t)

gam31z

γ(3)

1(z, t)

gam32z

γ(3)

2(z, t)

gam33z

γ(3)

3(z, t)

kap11z

κ11(z, t)

kap21z

κ21(z, t)

kap31z

κ31(z, t)

kap12z

κ12(z, t)

kap22z

κ22(z, t)

kap32z

κ32(z, t)

kap13z

κ13(z, t)

K.3 Parameters for ‘print.in’ 223

kap23z

κ23(z, t)

kap33z

κ33(z, t)

mgam33

˜γ33

mkap33

˜κ33

ngam33

ˆγ33

nkap33

ˆκ33

c1rms

hc2

1i1/2

c2rms

hc2

2i1/2

c3rms

hc2

3i1/2

c4rms

hc2

4i1/2

c5rms

hc2

5i1/2

c6rms

hc2

6i1/2

c1pt

c2pt

c3pt

c4pt

c5pt

c6pt

F11z

F21z

F31z

F12z

F22z

F32z

Module ‘testscalar_axisym.f90’

muc1

µ(c1)

muc2

µ(c2)

gamc

γ(c)

kapcPERP1

κ(1)

⊥

kapcPERP2

κ(2)

⊥

kapcPARA

κk

mucz

µ(c)(z, t)

gamcz

γ(c)(z, t)

kapcPERPz

κ⊥(z, t)

kapcPARAz

κk(z, t)

gam11

γ(1)

gam12

γ(1)

gam13

γ(1)

gam21

γ(2)

gam22

γ(2)

gam23

γ(2)

gam31

γ(3)

gam32

γ(3)

gam33

γ(3)

kap11

κ11

kap21

κ21

kap31

κ31

224 THE PENCIL CODE

kap12

κ12

kap22

κ22

kap32

κ32

kap13

κ13

kap23

κ23

kap33

κ33

gam11z

γ(1)

1(z, t)

gam12z

γ(1)

2(z, t)

gam13z

γ(1)

3(z, t)

gam21z

γ(2)

1(z, t)

gam22z

γ(2)

2(z, t)

gam23z

γ(2)

3(z, t)

gam31z

γ(3)

1(z, t)

gam32z

γ(3)

2(z, t)

gam33z

γ(3)

3(z, t)

gam3z

γ(c)(z, t)

kap11z

κ11(z, t)

kap21z

κ21(z, t)

kap31z

κ31(z, t)

kap12z

κ12(z, t)

kap22z

κ22(z, t)

kap32z

κ32(z, t)

kap13z

κ13(z, t)

kap23z

κ23(z, t)

kap33z

κ33(z, t)

mgam33

˜γ33

mkap33

˜κ33

ngam33

ˆγ33

nkap33

ˆκ33

c1rms

hc2

1i1/2

c2rms

hc2

2i1/2

c3rms

hc2

3i1/2

c4rms

hc2

4i1/2

c5rms

hc2

5i1/2

c6rms

hc2

6i1/2

c1pt

c2pt

c3pt

c4pt

c5pt

c6pt

F11z

F21z

F31z

F12z

F22z

F32z

Module ‘testscalar_simple.f90’

K.3 Parameters for ‘print.in’ 225

gam11

γ(1)

gam12

γ(1)

gam13

γ(1)

gam21

γ(2)

gam22

γ(2)

gam23

γ(2)

gam31

γ(3)

gam32

γ(3)

gam33

γ(3)

kap11

κ11

kap21

κ21

kap31

κ31

kap12

κ12

kap22

κ22

kap32

κ32

kap13

κ13

kap23

κ23

kap33

κ33

gam11z

γ(1)

1(z, t)

gam12z

γ(1)

2(z, t)

gam13z

γ(1)

3(z, t)

gam21z

γ(2)

1(z, t)

gam22z

γ(2)

2(z, t)

gam23z

γ(2)

3(z, t)

gam31z

γ(3)

1(z, t)

gam32z

γ(3)

2(z, t)

gam33z

γ(3)

3(z, t)

kap11z

κ11(z, t)

kap21z

κ21(z, t)

kap31z

κ31(z, t)

kap12z

κ12(z, t)

kap22z

κ22(z, t)

kap32z

κ32(z, t)

kap13z

κ13(z, t)

kap23z

κ23(z, t)

kap33z

κ33(z, t)

mgam33

˜γ33

mkap33

˜κ33

ngam33

ˆγ33

nkap33

ˆκ33

c1rms

hc2

1i1/2

c2rms

hc2

2i1/2

c3rms

hc2

3i1/2

c4rms

hc2

4i1/2

c5rms

hc2

5i1/2

c6rms

hc2

6i1/2

226 THE PENCIL CODE

c1pt

c2pt

c3pt

c4pt

c5pt

c6pt

F11z

F21z

F31z

F12z

F22z

F32z

Module ‘thermal_energy.f90’

TTmax

max(T)

TTmin

min(T)

ppm

hpi

TTm

hTi

ethm

hethi=hcvρT i(mean thermal energy)

ethtot

RVeth dV (total thermal energy)

ethmin

mineth

ethmax

maxeth

eem

hei=hcvTi(mean internal energy)

etot

heth +ρu2/2i

Module ‘visc_smagorinsky.f90’

nu LES

Mean value of Smagorinsky viscosity

Module ‘viscosity.f90’

nu tdep

time-dependent viscosity

fviscm

Mean value of viscous acceleration

fviscmin

Min value of viscous acceleration

fviscmax

Max value of viscous acceleration

fviscrmsx

Rms value of viscous acceleration for the vis xaver range

num

Mean value of viscosity

nusmagm

Mean value of Smagorinsky viscosity

nusmagmin

Min value of Smagorinsky viscosity

nusmagmax

Max value of Smagorinsky viscosity

nu LES

Mean value of Smagorinsky viscosity

visc heatm

Mean value of viscous heating

qfviscm

hq·fvisci

ufviscm

hu·fvisci

Sij2m

S2

epsK

2ν̺S2

slope c max

Max value of characteric speed of slope limited diffusion

dtnu

δt/[cδt,vδx2/νmax](time step relative to viscous time step; see

§5.15)

meshRemax

Max mesh Reynolds number

Reshock

Mesh Reynolds number at shock

K.4 Parameters for ‘video.in’ 227

K.4 List of parameters for ‘video.in’

The following table lists all (at the time of writing, December 23, 2018) possible inputs

to the ﬁle ‘video.in’.

Variable Meaning

Module ‘hydro.f90’

velocity vector u; writes all three components separately to

ﬁles ‘u[xyz].{xz,yz,xy,xy2}’

kinetic energy density u2; writes ‘u2.{xz,yz,xy,xy2}’

vorticity vector ω=∇ × u; writes all three components sepa-

rately to ﬁles ‘oo[xyz].{xz,yz,xy,xy2}’

enstrophy ω2=|∇ × u|2; writes ‘o2.{xz,yz,xy,xy2}’

divu

∇·u; writes ‘divu.{xz,yz,xy,xy2}’

mach

Mach number squared Ma2; writes ‘mach.{xz,yz,xy,xy2}’

Module ‘density.f90’

lnrho

logarithmic density ln ρ; writes ‘lnrho.{xz,yz,xy,xy2}’

rho

density ρ; writes ‘rho.{xz,yz,xy,xy2}’

Module ‘entropy.f90’

entropy s; writes ‘ss.{xz,yz,xy,xy2}’

pressure p; writes ‘pp.{xz,yz,xy,xy2}’

Module ‘temperature_idealgas.f90’

lnTT

logarithmic temperature ln T; writes ‘lnTT.{xz,yz,xy,xy2}’

temperature T; writes ‘TT.{xz,yz,xy,xy2}’

Module ‘shock.f90’

shock

shock viscosity νshock; writes ‘shock.{xz,yz,xy,xy2}’

Module ‘eos_ionization.f90’

ionization fraction yH; writes ‘yH.{xz,yz,xy,xy2}’

Module ‘radiation_ray.f90’

Qrad

radiative heating rate Qrad; writes ‘Qrad.{xz,yz,xy,xy2}’

Isurf

surface intensity Isurf (?); writes ‘Isurf.xz’

Module ‘magnetic.f90’

magnetic vector potential A; writes ‘aa[xyz].{xz,yz,xy,xy2}’

magnetic ﬂux density B; writes ‘bb[xyz].{xz,yz,xy,xy2}’

magnetic energy density B2; writes ‘b2.{xz,yz,xy,xy2}’

current density j; writes ‘jj[xyz].{xz,yz,xy,xy2}’

current density squared j2; writes ‘j2.{xz,yz,xy,xy2}’

jB; writes ‘jb.{xz,yz,xy,xy2}’

beta1

inverse plasma beta B2/(2µ0p); writes ‘beta1.{xz,yz,xy,xy2}’

Poynting

Poynting vector ηj×B−(u×B)×B/µ0; writes

‘Poynting[xyz].{xz,yz,xy,xy2}’

228 THE PENCIL CODE

magnetic helicity density A·B; writes

‘ab[xyz].{xz,yz,xy,xy2}’

Module ‘pscalar.f90’

lncc

logarithmic density of passive scalar ln c; writes

‘lncc.{xz,yz,xy,xy2}’

Module ‘cosmicray.f90’

ecr

energy ecr of cosmic rays (?); writes ‘ec.{xz,yz,xy,xy2}’

K.5 List of parameters for ‘phiaver.in’

The following table lists all (at the time of writing, November 2003) possible inputs to

the ﬁle ‘phiaver.in’.

Variable Meaning

Module ‘cdata.f90’

rcylmphi

cylindrical radius ̟=px2+y2(useful for debugging az-

imuthal averages)

phimphi

azimuthal angle ϕ= arctan y

x(useful for debugging)

zmphi

z-coordinate (useful for debugging)

rmphi

spherical radius r=√̟2+z2(useful for debugging)

Module ‘hydro.f90’

urmphi

hu̟iϕ[cyl. polar coords (̟, ϕ, z)]

upmphi

huϕiϕ

uzmphi

huziϕ

ursphmphi

huriϕ

uthmphi

huϑiϕ

uumphi

shorthand for

urmphi

upmphi

and

uzmphi

together

uusphmphi

shorthand for

ursphmphi

uthmphi

and

upmphi

together

u2mphi

hu2iϕ

Module ‘density.f90’

lnrhomphi

hln ̺iϕ

rhomphi

h̺iϕ

Module ‘entropy.f90’

ssmphi

hsiϕ

cs2mphi

hc2

siϕ

Module ‘magnetic.f90’

jbmphi

hJ·Biϕ

brmphi

hB̟iϕ[cyl. polar coords (̟, ϕ, z)]

bpmphi

hBϕiϕ

bzmphi

hBziϕ

bbmphi

shorthand for

brmphi

bpmphi

and

bzmphi

together

K.6 Parameters for ‘xyaver.in’ 229

bbsphmphi

shorthand for

brsphmphi

bthmphi

and

bpmphi

together

b2mphi

B2ϕ

brsphmphi

hBriϕ

bthmphi

hBϑiϕ

Module ‘anelastic.f90’

lnrhomphi

hln ̺iϕ

rhomphi

h̺iϕ

Module ‘entropy_anelastic.f90’

ssmphi

hsiϕ

cs2mphi

hc2

siϕ

Module ‘magnetic_shearboxJ.f90’

jbmphi

hJ·Biϕ

brmphi

hB̟iϕ[cyl. polar coords (̟, ϕ, z)]

bpmphi

hBϕiϕ

bzmphi

hBziϕ

bbmphi

shorthand for

brmphi

bpmphi

and

bzmphi

together

bbsphmphi

shorthand for

brsphmphi

bthmphi

and

bpmphi

together

b2mphi

B2ϕ

brsphmphi

hBriϕ

bthmphi

hBϑiϕ

K.6 List of parameters for ‘xyaver.in’

The following table lists possible inputs to the ﬁle ‘xyaver.in’. This list is not complete

and maybe outdated.

Variable Meaning

Module ‘hydro.f90’

u2mz

hu2ixy

o2mz

W2xy

divu2mz

h(∇ · u)2ixy

curlru2mz

h(∇ × ̺U)2ixy

divru2mz

h(∇ · ̺u)2ixy

fmasszmz

h̺uzixy

fkinzmz

1

2̺u2uzxy

uxmz

huxixy (horiz. averaged xvelocity)

uymz

huyixy

uzmz

huzixy

uzupmz

huz↑ixy

uzdownmz

huz↓ixy

ruzupmz

h̺uz↑ixy

ruzdownmz

h̺uz↓ixy

divumz

hdivuixy

230 THE PENCIL CODE

uzdivumz

huzdivuixy

oxmz

hωxixy

oymz

hωyixy

ozmz

hωzixy

ux2mz

hu2

xixy

uy2mz

u2

yxy

uz2mz

hu2

zixy

ox2mz

hω2

xixy

oy2mz

ω2

yxy

oz2mz

hω2

zixy

ruxmz

h̺uxixy

ruymz

h̺uyixy

ruzmz

h̺uzixy

rux2mz

h̺u2

xixy

ruy2mz

̺u2

yxy

ruz2mz

h̺u2

zixy

uxuymz

huxuyixy

uxuzmz

huxuzixy

uyuzmz

huyuzixy

ruxuymz

hρuxuyixy

ruxuzmz

hρuxuzixy

ruyuzmz

hρuyuzixy

ruxuy2mz

hρuxuyixy

ruxuz2mz

hρuxuzixy

ruyuz2mz

hρuyuzixy

oxuxxmz

hωxux,xixy

oyuxymz

hωyux,yixy

oxuyxmz

hωxuy,xixy

oyuyymz

hωyuy,yixy

oxuzxmz

hωxuz,xixy

oyuzymz

hωyuz,yixy

uyxuzxmz

huy,xuz,xixy

uyyuzymz

huy,yuz,yixy

uyzuzzmz

huy,zuz,zixy

ekinmz

1

2̺u2xy

oumz

hω·uixy

Remz

h|u·u|



∂

∂xj(νSij )



ixy

oguxmz

h(ω· ∇u)xixy

oguymz

h(ω· ∇u)yixy

oguzmz

h(ω· ∇u)zixy

ogux2mz

h(ω· ∇u)2

xixy

oguy2mz

(ω· ∇u)2

yxy

oguz2mz

h(ω· ∇u)2

zixy

oxdivumz

hωx∇ · uixy

oydivumz

hωy∇ · uixy

ozdivumz

hωz∇ · uixy

K.6 Parameters for ‘xyaver.in’ 231

oxdivu2mz

h(ωxnabla ·u)2ixy

oydivu2mz

h(ωy∇ · u)2ixy

ozdivu2mz

h(ωz∇ · u)2ixy

accpowzmz

h(uzDuz/Dt)2ixy

accpowzupmz

h(uzDuz/Dt)2ixy+

accpowzdownmz

h(uzDuz/Dt)2ixy−

fkinxmx

1

2̺u2uxyz

Module ‘density.f90’

rhomz

h̺ixy

rho2mz

h̺2ixy

gzlnrhomz

h∇zln ̺ixy

uglnrhomz

hu· ∇ln ̺ixy

ugrhomz

hu· ∇̺ixy

uygzlnrhomz

huy∇zln ̺ixy

uzgylnrhomz

huz∇yln ̺ixy

rho2mx

h̺2iyz

Module ‘entropy.f90’

fradz

hFradixy

fconvz

hcp̺uzTixy

ssmz

hsixy

ss2mz

hs2ixy

ppmz

hpixy

TTmz

hTixy

TT2mz

hT2ixy

uxTTmz

huxTixy

uyTTmz

huyTixy

uzTTmz

huzTixy

gTxgsxmz

h(∇T× ∇s)xixy

gTxgsymz

h(∇T× ∇s)yixy

gTxgszmz

h(∇T× ∇s)zixy

gTxgsx2mz

h(∇T× ∇s)2

xixy

gTxgsy2mz

(∇T× ∇s)2

yxy

gTxgsz2mz

h(∇T× ∇s)2

zixy

fradz kramers

Frad (from Kramers’ opacity)

fradz Kprof

Frad (from Kprof)

fradz constchi

Frad (from chi const)

fturbz

h̺T χt∇zsixy (turbulent heat ﬂux)

fturbtz

h̺T χt0∇zsixy (turbulent heat ﬂux)

fturbmz

h̺T χt0∇zsixy (turbulent heat ﬂux)

fturbfz

h̺T χt0∇zs′ixy (turbulent heat ﬂux)

dcoolz

surface cooling ﬂux

heatmz

heating

Kkramersmz

K0T(3−b)/rho(a+ 1)xy

ethmz

h̺eixy

Module ‘magnetic.f90’

232 THE PENCIL CODE

axmz

hAxixy

aymz

hAyixy

azmz

hAzixy

abuxmz

h(A·B)uxixy

abuymz

h(A·B)uyixy

abuzmz

h(A·B)uzixy

uabxmz

h(u·A)Bxixy

uabymz

h(u·A)Byixy

uabzmz

h(u·A)Bzixy

bbxmz

hB′

xixy

bbymz

B′

yxy

bbzmz

hB′

zixy

bxmz

hBxixy

bymz

hByixy

bzmz

hBzixy

jxmz

hJxixy

jymz

hJyixy

jzmz

hJzixy

Exmz

hExixy

Eymz

hEyixy

Ezmz

hEzixy

bx2mz

hB2

xixy

by2mz

B2

yxy

bz2mz

hB2

zixy

bx2rmz

hB2

x/̺ixy

by2rmz

B2

y/̺xy

bz2rmz

hB2

z/̺ixy

beta1mz

h(B2/2µ0)/pixy

betamz

hβixy

beta2mz

hβ2ixy

jbmz

hJ·Bi|xy

d6abmz

h∇6A·Bi|xy

d6amz1

h∇6Aixy |x

d6amz2

h∇6Aixy |y

d6amz3

h∇6Aixy |z

abmz

hA·Bi|xy

ubmz

hu·Bi|xy

uamz

hu·Ai|xy

uxbxmz

huxbxi|xy

uybxmz

huybxi|xy

uzbxmz

huzbxi|xy

uxbymz

huxbyi|xy

uybymz

huybyi|xy

uzbymz

huzbyi|xy

uxbzmz

huxbzi|xy

uybzmz

huybzi|xy

uzbzmz

huzbzi|xy

examz1

hE×Aixy |x

K.6 Parameters for ‘xyaver.in’ 233

examz2

hE×Aixy |y

examz3

hE×Aixy |z

e3xamz1

hEhyper3×Aixy |x

e3xamz2

hEhyper3×Aixy |y

e3xamz3

hEhyper3×Aixy |z

etatotalmz

hηixy

bxbymz

hBxByixy

bxbzmz

hBxBzixy

bybzmz

hByBzixy

b2mz

B2xy

bf2mz

B′2xy

j2mz

j2xy

poynzmz

Averaged poynting ﬂux in z direction

epsMmz

ηµ0j2xy

vmagfricmz

1/νmag|j×B/B2|xy

Module ‘bfield.f90’

bmz

hBixy

b2mz

hB2ixy

bxmz

hBxixy

bymz

hByixy

bzmz

hBzixy

bx2mz

hB2

xixy

by2mz

hB2

yixy

bz2mz

hB2

zixy

bxbymz

hBxByixy

bxbzmz

hBxBzixy

bybzmz

hByBzixy

betamz

hβixy

beta2mz

hβ2ixy

Module ‘density_stratified.f90’

drhomz

h∆ρ/ρ0ixy

drho2mz

h(∆ρ/ρ0)2ixy

Module ‘gravity_simple.f90’

epotmz

h̺Φgravixy

epotuzmz

h̺Φgravuzixy (potential energy ﬂux)

Module ‘magnetic_shearboxJ.f90’

axmz

hAxixy

aymz

hAyixy

azmz

hAzixy

abuxmz

h(A·B)uxixy

abuymz

h(A·B)uyixy

abuzmz

h(A·B)uzixy

uabxmz

h(u·A)Bxixy

uabymz

h(u·A)Byixy

uabzmz

h(u·A)Bzixy

234 THE PENCIL CODE

bbxmz

hB′

xixy

bbymz

B′

yxy

bbzmz

hB′

zixy

bxmz

hBxixy

bymz

hByixy

bzmz

hBzixy

jxmz

hJxixy

jymz

hJyixy

jzmz

hJzixy

Exmz

hExixy

Eymz

hEyixy

Ezmz

hEzixy

bx2mz

hB2

xixy

by2mz

B2

yxy

bz2mz

hB2

zixy

bx2rmz

hB2

x/̺ixy

by2rmz

B2

y/̺xy

bz2rmz

hB2

z/̺ixy

beta1mz

h(B2/2µ0)/pixy

betamz

hβixy

beta2mz

hβ2ixy

jbmz

hJ·Bi|xy

d6abmz

h∇6A·Bi|xy

d6amz1

h∇6Aixy |x

d6amz2

h∇6Aixy |y

d6amz3

h∇6Aixy |z

abmz

hA·Bi|xy

ubmz

hu·Bi|xy

uamz

hu·Ai|xy

uxbxmz

huxbxi|xy

uybxmz

huybxi|xy

uzbxmz

huzbxi|xy

uxbymz

huxbyi|xy

uybymz

huybyi|xy

uzbymz

huzbyi|xy

uxbzmz

huxbzi|xy

uybzmz

huybzi|xy

uzbzmz

huzbzi|xy

examz1

hE×Aixy |x

examz2

hE×Aixy |y

examz3

hE×Aixy |z

e3xamz1

hEhyper3×Aixy |x

e3xamz2

hEhyper3×Aixy |y

e3xamz3

hEhyper3×Aixy |z

etatotalmz

hηixy

bxbymz

hBxByixy

bxbzmz

hBxBzixy

bybzmz

hByBzixy

K.7 Parameters for ‘xzaver.in’ 235

b2mz

B2xy

bf2mz

B′2xy

j2mz

j2xy

poynzmz

Averaged poynting ﬂux in z direction

epsMmz

ηµ0j2xy

Module ‘meanfield.f90’

qpmz

hqpixy

Module ‘shock_highorder.f90’

Module ‘temperature_idealgas.f90’

ppmz

hpixy

TTmz

hTixy

ethmz

hethixy

fpresxmz

h(∇p)xixy

fpresymz

h(∇p)yixy

fpreszmz

h(∇p)zixy

TT2mz

hT2ixy

uxTmz

huxTixy

uyTmz

huyTixy

uzTmz

huzTixy

fradmz

hFradixy

fconvmz

hcp̺uzTixy

Module ‘temperature_ionization.f90’

puzmz

hpuzixy

pr1mz

hp/̺ixy

eruzmz

he̺uzixy

ffakez

h̺uzcpTixy

mumz

hµixy

TTmz

hTixy

ssmz

hsixy

eemz

heixy

ppmz

hpixy

Module ‘thermal_energy.f90’

ppmz

hpixy

TTmz

hTixy

Module ‘viscosity.f90’

fviscmz

h2ν̺uiSizixy (z-component of viscous ﬂux)

fviscsmmz

h2νSmag̺uiSiz ixy (z-component of viscous ﬂux)

epsKmz

2ν̺S2xy

K.7 List of parameters for ‘xzaver.in’

236 THE PENCIL CODE

The following table lists possible inputs to the ﬁle ‘xzaver.in’. This list is not complete

and maybe outdated.

Variable Meaning

Module ‘hydro.f90’

uxmy

huxixz

uymy

huyixz

uzmy

huzixz

oumy

hω·uixz

Module ‘density.f90’

rhomy

h̺ixz

Module ‘entropy.f90’

ssmy

hsixz

ppmy

hpixz

TTmy

hTixz

Module ‘magnetic.f90’

bxmy

hBxixz

bymy

hByixz

bzmy

hBzixz

bx2my

hB2

xixz

by2my

B2

yxz

bz2my

hB2

zixz

bxbymy

hBxByixz

bxbzmy

hBxBzixz

bybzmy

hByBzixz

Module ‘density_stratified.f90’

drhomy

h∆ρ/ρ0ixz

drho2my

h(∆ρ/ρ0)2ixz

Module ‘gravity_simple.f90’

epotmy

h̺Φgravixz

Module ‘magnetic_shearboxJ.f90’

bxmy

hBxixz

bymy

hByixz

bzmy

hBzixz

bx2my

hB2

xixz

by2my

B2

yxz

bz2my

hB2

zixz

bxbymy

hBxByixz

bxbzmy

hBxBzixz

bybzmy

hByBzixz

Module ‘shock_highorder.f90’

Module ‘temperature_idealgas.f90’

ppmy

hpixz

K.8 Parameters for ‘yzaver.in’ 237

TTmy

hTixz

Module ‘thermal_energy.f90’

ppmy

hpixz

TTmy

hTixz

K.8 List of parameters for ‘yzaver.in’

The following table lists possible inputs to the ﬁle ‘yzaver.in’. This list is not complete

and maybe outdated.

Variable Meaning

Module ‘hydro.f90’

uxmx

huxiyz

uymx

huyiyz

uzmx

huziyz

ruxmx

h̺uxiyz

ruymx

h̺uyiyz

ruzmx

h̺uziyz

rux2mx

hρu2

xiyz

ruy2mx

hρu2

yiyz

ruz2mx

hρu2

ziyz

ruxuymx

hρuxuyiyz

ruxuzmx

hρuxuziyz

ruyuzmx

hρuyuziyz

ux2mx

hu2

xiyz

uy2mx

u2

yyz

uz2mx

hu2

ziyz

ox2mx

hω2

xiyz

oy2mx

ω2

yyz

oz2mx

hω2

ziyz

uxuymx

huxuyiyz

uxuzmx

huxuziyz

uyuzmx

huyuziyz

oumx

hω·uiyz

ekinmx

2ρu2ixy

Module ‘density.f90’

rhomx

h̺iyz

Module ‘entropy.f90’

ssmx

hsiyz

ss2mx

hs2iyz

ppmx

hpiyz

TTmx

hTiyz

TT2mx

hT2iyz

238 THE PENCIL CODE

uxTTmx

huxTiyz

uyTTmx

huyTiyz

uzTTmx

huzTiyz

fconvxmx

hcp̺uxTiyz

fradmx

hFradiyz

fturbmx

h̺T χt∇xsiyz (turbulent heat ﬂux)

Kkramersmx

K0T(3−b)/rho(a+ 1)yz

dcoolx

surface cooling ﬂux

fradx kramers

Frad (from Kramers’ opacity)

Module ‘magnetic.f90’

b2mx

hB2iyz

bxmx

hBxiyz

bymx

hByiyz

bzmx

hBziyz

bx2mx

hB2

xiyz

by2mx

B2

yyz

bz2mx

hB2

ziyz

bxbymx

hBxByiyz

bxbzmx

hBxBziyz

bybzmx

hByBziyz

betamx

hβiyz

beta2mx

hβ2iyz

etatotalmx

hηiyz

Module ‘bfield.f90’

bmx

hBiyz

b2mx

hB2iyz

bxmx

hBxiyz

bymx

hByiyz

bzmx

hBziyz

bx2mx

hB2

xiyz

by2mx

hB2

yiyz

bz2mx

hB2

ziyz

bxbymx

hBxByiyz

bxbzmx

hBxBziyz

bybzmx

hByBziyz

betamx

hβiyz

beta2mx

hβ2iyz

Module ‘density_stratified.f90’

drhomx

h∆ρ/ρ0iyz

drho2mx

h(∆ρ/ρ0)2iyz

Module ‘gravity_simple.f90’

epotmx

h̺Φgraviyz

epotuxmx

h̺Φgravuxiyz (potential energy ﬂux)

Module ‘magnetic_shearboxJ.f90’

b2mx

hB2iyz

K.9 Parameters for ‘yaver.in’ 239

bxmx

hBxiyz

bymx

hByiyz

bzmx

hBziyz

bx2mx

hB2

xiyz

by2mx

B2

yyz

bz2mx

hB2

ziyz

bxbymx

hBxByiyz

bxbzmx

hBxBziyz

bybzmx

hByBziyz

betamx

hβiyz

beta2mx

hβ2iyz

etatotalmx

hηiyz

Module ‘shock_highorder.f90’

Module ‘temperature_idealgas.f90’

ppmx

hpiyz

TTmx

hTiyz

Module ‘thermal_energy.f90’

ppmx

hpiyz

TTmx

hTiyz

Module ‘viscosity.f90’

fviscmx

h2ν̺uiSixiyz (x-component of viscous ﬂux)

numx

hνiyz (yz-averaged viscosity)

K.9 List of parameters for ‘yaver.in’

The following table lists possible inputs to the ﬁle ‘yaver.in’. This list is not complete

and maybe outdated.

Variable Meaning

Module ‘hydro.f90’

uxmxz

huxiy

uymxz

huyiy

uzmxz

huziy

ux2mxz

hu2

xiy

uy2mxz

u2

yy

uz2mxz

hu2

ziy

uxuymxz

huxuyiy

uxuzmxz

huxuziy

uyuzmxz

huyuziy

oumxz

hω·uiy

Module ‘density.f90’

rhomxz

h̺iy

240 THE PENCIL CODE

Module ‘entropy.f90’

TTmxz

hTiy

ssmxz

hsiy

Module ‘magnetic.f90’

b2mxz

B2y

axmxz

hAxiy

aymxz

hAyiy

azmxz

hAziy

bx1mxz

h|Bx|iy

by1mxz

h|By|iy

bz1mxz

h|Bz|iy

bxmxz

hBxiy

bymxz

hByiy

bzmxz

hBziy

jxmxz

hJxiy

jymxz

hJyiy

jzmxz

hJziy

bx2mxz

hB2

xiy

by2mxz

B2

yy

bz2mxz

hB2

ziy

bxbymxz

hBxByiy

bxbzmxz

hBxBziy

bybzmxz

hByBziy

uybxmxz

hUyBxiy

uybzmxz

hUyBziy

Exmxz

hExiy

Eymxz

hEyiy

Ezmxz

hEziy

vAmxz

hv2

Aiy

Module ‘density_stratified.f90’

drhomxz

h∆ρ/ρ0iy

drho2mxz

h(∆ρ/ρ0)2iy

Module ‘magnetic_shearboxJ.f90’

b2mxz

B2y

axmxz

hAxiy

aymxz

hAyiy

azmxz

hAziy

bx1mxz

h|Bx|iy

by1mxz

h|By|iy

bz1mxz

h|Bz|iy

bxmxz

hBxiy

bymxz

hByiy

bzmxz

hBziy

jxmxz

hJxiy

K.10 Parameters for ‘zaver.in’ 241

jymxz

hJyiy

jzmxz

hJziy

bx2mxz

hB2

xiy

by2mxz

B2

yy

bz2mxz

hB2

ziy

bxbymxz

hBxByiy

bxbzmxz

hBxBziy

bybzmxz

hByBziy

uybxmxz

hUyBxiy

uybzmxz

hUyBziy

Exmxz

hExiy

Eymxz

hEyiy

Ezmxz

hEziy

vAmxz

hv2

Aiy

Module ‘meanfield.f90’

peffmxz

hPeﬀ iy

alpmxz

hαiy

Module ‘temperature_idealgas.f90’

TTmxz

hTiy

Emymxz

hEmyiyEmission in y-direction

Module ‘thermal_energy.f90’

TTmxz

hTiy

K.10 List of parameters for ‘zaver.in’

The following table lists possible inputs to the ﬁle ‘zaver.in’. This list is not complete

and maybe outdated.

Variable Meaning

Module ‘hydro.f90’

uxmxy

huxiz

uymxy

huyiz

uzmxy

huziz

uxuymxy

huxuyiz

uxuzmxy

huxuziz

uyuzmxy

huyuziz

oxmxy

hωxiz

oymxy

hωyiz

ozmxy

hωziz

oumxy

hω·uiz

pvzmxy

h(ωz+ 2Ω)/̺iz(z component of potential vorticity)

uguxmxy

h(u·∇u)xiz

uguymxy

h(u·∇u)yiz

242 THE PENCIL CODE

uguzmxy

h(u·∇u)ziz

ruxmxy

hρuxiz

ruymxy

hρuyiz

ruzmxy

hρuziz

ux2mxy

hu2

xiz

uy2mxy

u2

yz

uz2mxy

hu2

ziz

rux2mxy

hρu2

xiz

ruy2mxy

ρu2

yz

ruz2mxy

hρu2

ziz

ruxuymxy

hρuxuyiz

ruxuzmxy

hρuxuziz

ruyuzmxy

hρuyuziz

fkinxmxy

1

2̺u2uxz

fkinymxy

1

2̺u2uyz

Module ‘density.f90’

rhomxy

h̺iz

Module ‘entropy.f90’

TTmxy

hTiz

ssmxy

hsiz

uxTTmxy

huxTiz

uyTTmxy

huyTiz

uzTTmxy

huzTiz

gTxmxy

h∇xTiz

gTymxy

h∇yTiz

gTzmxy

h∇zTiz

gsxmxy

h∇xsiz

gsymxy

h∇ysiz

gszmxy

h∇zsiz

gTxgsxmxy

h(∇T× ∇s)xiz

gTxgsymxy

D(∇T× ∇s)yEz

gTxgszmxy

h(∇T× ∇s)ziz

gTxgsx2mxy

(∇T× ∇s)2

xz

gTxgsy2mxy

D(∇T× ∇s)2

yEz

gTxgsz2mxy

(∇T× ∇s)2

zz

fconvxy

hcp̺uxTiz

fconvyxy

hcp̺uyTiz

fconvzxy

hcp̺uzTiz

fradxy Kprof

Frad

x(x-component of radiative ﬂux, z-averaged, from Kprof)

fradymxy Kprof

Frad

y(y-component of radiative ﬂux, z-averaged, from Kprof)

fradxy kramers

Frad (z-averaged, from Kramers’ opacity)

fturbxy

h̺T χt∇xsiz

fturbymxy

h̺T χt∇ysiz

fturbrxy

h̺T χri∇isiz(radial part of anisotropic turbulent heat ﬂux)

fturbthxy

h̺T χθi∇isiz(latitudinal part of anisotropic turbulent heat

ﬂux)

dcoolxy

surface cooling ﬂux

K.10 Parameters for ‘zaver.in’ 243

Module ‘magnetic.f90’

bxmxy

hBxiz

bymxy

hByiz

bzmxy

hBziz

jxmxy

hJxiz

jymxy

hJyiz

jzmxy

hJziz

axmxy

hAxiz

aymxy

hAyiz

azmxy

hAziz

bx2mxy

hB2

xiz

by2mxy

B2

yz

bz2mxy

hB2

ziz

bxbymxy

hBxByiz

bxbzmxy

hBxBziz

bybzmxy

hByBziz

poynxmxy

hE×Bix

poynymxy

hE×Biy

poynzmxy

hE×Biz

jbmxy

hJ·Biz

abmxy

hA·Biz

examxy1

hE×Aiz|x

examxy2

hE×Aiz|y

examxy3

hE×Aiz|z

StokesImxy

hǫB⊥iz|z

StokesQmxy

−hǫB⊥cos 2χiz|z

StokesUmxy

−hǫB⊥sin 2χiz|z

StokesQ1mxy

+hF ǫB⊥sin 2χiz|z

StokesU1mxy

−hF ǫB⊥cos 2χiz|z

beta1mxy

B2/(2µ0p)z|z

Module ‘density_stratified.f90’

drhomxy

h∆ρ/ρ0iz

drho2mxy

h(∆ρ/ρ0)2iz

Module ‘gravity_simple.f90’

epotmxy

h̺Φgraviz

epotuxmxy

h̺Φgravuxiz(potential energy ﬂux)

Module ‘magnetic_shearboxJ.f90’

bxmxy

hBxiz

bymxy

hByiz

bzmxy

hBziz

jxmxy

hJxiz

jymxy

hJyiz

jzmxy

hJziz

axmxy

hAxiz

aymxy

hAyiz

azmxy

hAziz

bx2mxy

hB2

xiz

244 THE PENCIL CODE

by2mxy

B2

yz

bz2mxy

hB2

ziz

bxbymxy

hBxByiz

bxbzmxy

hBxBziz

bybzmxy

hByBziz

poynxmxy

hE×Bix

poynymxy

hE×Biy

poynzmxy

hE×Biz

jbmxy

hJ·Biz

abmxy

hA·Biz

examxy1

hE×Aiz|x

examxy2

hE×Aiz|y

examxy3

hE×Aiz|z

StokesImxy

hǫB⊥iz|z

StokesQmxy

−hǫB⊥cos 2χiz|z

StokesUmxy

−hǫB⊥sin 2χiz|z

StokesQ1mxy

+hF ǫB⊥sin 2χiz|z

StokesU1mxy

−hF ǫB⊥cos 2χiz|z

beta1mxy

B2/(2µ0p)z|z

Module ‘temperature_idealgas.f90’

TTmxy

hTiz

Emzmxy

hEmzizEmission in z-direction

Module ‘thermal_energy.f90’

TTmxy

hTiz

Module ‘viscosity.f90’

fviscmxy

h2ν̺uiSixiz(x-xomponent of viscous ﬂux)

fviscsmmxy

h2νSmag̺uiSixiz(x-xomponent of viscous ﬂux)

fviscymxy

h2ν̺uiSiyiz(y-xomponent of viscous ﬂux)

K.11 Boundary conditions

The following tables list all possible boundary condition labels that are documented.

K.11.1 Boundary condition

bcx

Variable Meaning

Module ‘boundcond.f90’

zero value in ghost zones, free value on boundary

periodic

symmetry, fN+i=fN−i; implies f′(xN) = f′′′(x0) = 0

symmetry with respect to interface

symmetry, plus function value given

s0d

symmetry, function value such that df/dx=0

antisymmetry, fN+i=−fN−i; implies f(xN) = f′′(x0) = 0

antisymmetry with respect to interface

K.11 Boundary conditions 245

antisymmetry relative to boundary value, fN+i= 2fN−fN−i; implies

f′′(x0) = 0

a2v

set boundary value and antisymmetry relative to it fN+i= 2fN−fN−i;

implies f′′(x0) = 0

a2r

sets d2f/dr2+ 2df/dr −2f/r2= 0 This is the replacement of zero second

derivative in spherical coordinates, in radial direction.

cpc

cylindrical perfect conductor implies f′′ +f′/R = 0

cpp

cylindrical perfect conductor implies f′′ +f′/R = 0

cpz

cylindrical perfect conductor implies f′′ +f′/R = 0

spr

spherical perfect conductor implies f′′ + 2f′/R = 0 and f(xN) = 0

vanishing third derivative

cop

copy value of last physical point to all ghost cells

onesided

d1s

onesided for 1st/2nd derivative in two ﬁrst inner points, Dirichlet in

boundary point

n1s

onesided for 1st/2nd derivative in two ﬁrst inner points, Neumann in

boundary point

1so

onesided

constant temperature (implemented as condition for entropy sor tem-

perature T)

constant temperature (or maybe rather constant conductive ﬂux??)

Fgs

Fconv = - chi t*rho*T*grad(s)

Fct

Fbot = - K*grad(T) - chi t*rho*T*grad(s)

Fcm

F bot =−K∗grad(T)−chit∗rho ∗T∗grad(s)

symmetric temperature, TN−i=TN+i; implies T′(xN) = T′′′(x0) = 0

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

“freeze” value, i.e. maintain initial

f= 1 (for debugging)

set

set boundary value to

fbcx

der

set derivative on boundary to

fbcx

slo

set slope at the boundary =

fbcx

slp

set slope at the boundary and in ghost cells =

fbcx

shx

set shearing boundary proportional to x with slope=

fbcx

and ab-

scissa=

fbcx2

shy

set shearing boundary proportional to y with slope=

fbcx

and ab-

scissa=

fbcx2

shz

set shearing boundary proportional to z with slope=

fbcx

and ab-

scissa=

fbcx2

dr0

set boundary value [really??]

ovr

overshoot boundary condition ie (d/dx −1/dist)f= 0.

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

e1o

allow outﬂow, but no inﬂow uses the e1 extrapolation scheme

ant

stops and prompts for adding documentation

extrapolation [describe]

extrapolation in log [maintain a power law]

linear extrapolation from last two active cells

246 THE PENCIL CODE

hat

top hat jet proﬁle in spherical coordinate.

jet

top hat jet proﬁle in cartezian coordinate.

spd

sets d(rAα)/dr =fbcx(j)

sfr

stress-free boundary condition for spherical coordinate system.

sr1

Stress-free bc for spherical coordinate system. Implementation with

one-sided derivative.

nfr

Normal-ﬁeld bc for spherical coordinate system. Some people call this

the “(angry) hedgehog bc”.

nr1

Normal-ﬁeld bc for spherical coordinate system. Some people call this

the “(angry) hedgehog bc”. Implementation with one-sided derivative.

sa2

(d/dr)(rBφ) = 0 imposes boundary condition on 2nd derivative of rAφ.

Same applies to θcomponent.

pfc

perfect-conductor in spherical coordinate: d/dr(Ar) + 2/r = 0.

ﬁx

set boundary value [really??]

ﬁl

set boundary value from a ﬁle

cfb

radial centrifugal balance

set to given value(s) or function

nil

do nothing; assume that everything is set

ioc

inlet/outlet on western/eastern hemisphere in cylindrical coordinates

do nothing; assume that everything is set

implies f′(yN) = f′′′(y0) = 0

Module ‘boundcond_alt.f90’

zero value in ghost zones, free value on boundary

periodic

symmetry, fN+i=fN−i; implies f′(xN) = f′′′(x0) = 0

symmetry, plus function value given

s0d

symmetry, function value such that df/dx=0

antisymmetry, fN+i=−fN−i; implies f(xN) = f′′(x0) = 0

antisymmetry relative to boundary value, fN+i= 2fN−fN−i; implies

f′′(x0) = 0

a2r

sets d2f/dr2+ 2df/dr −2f/r2= 0 This is the replacement of zero second

derivative in spherical coordinates, in radial direction.

cpc

cylindrical perfect conductor implies f′′ +f′/R = 0

cpp

cylindrical perfect conductor implies f′′ +f′/R = 0

cpz

cylindrical perfect conductor implies f′′ +f′/R = 0

spr

spherical perfect conductor implies f′′ + 2f′/R = 0 and f(xN) = 0

vanishing third derivative

cop

copy value of last physical point to all ghost cells

onesided

1so

onesided

constant temperature (implemented as condition for entropy sor tem-

perature T)

constant temperature (or maybe rather constant conductive ﬂux??)

Fgs

Fconv = - chi t*rho*T*grad(s)

Fct

Fbot = - K*grad(T) - chi t*rho*T*grad(s)

Fcm

F bot =−K∗grad(T)−chit∗rho ∗T∗grad(s)

symmetric temperature, TN−i=TN+i; implies T′(xN) = T′′′(x0) = 0

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

K.11 Boundary conditions 247

“freeze” value, i.e. maintain initial

f= 1 (for debugging)

set

set boundary value to

fbcx12

der

set derivative on boundary to

fbcx12

slo

set slope at the boundary =

fbcx12

dr0

set boundary value [really??]

ovr

overshoot boundary condition ie (d/dx −1/dist)f= 0.

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

e1o

allow outﬂow, but no inﬂow uses the e1 extrapolation scheme

ant

stops and prompts for adding documentation

extrapolation [describe]

extrapolation in log [maintain a power law]

hat

top hat jet proﬁle in spherical coordinate.

jet

top hat jet proﬁle in cartezian coordinate.

spd

sets d(rAα)/dr =fbcx12(j)

sfr

stress-free boundary condition for spherical coordinate system.

nfr

Normal-ﬁeld bc for spherical coordinate system. Some people call this

the “(angry) hedgehog bc”.

sa2

(d/dr)(rBφ) = 0 imposes boundary condition on 2nd derivative of rAφ.

Same applies to θcomponent.

pfc

perfect-conductor in spherical coordinate: d/dr(Ar) + 2/r = 0.

ﬁx

set boundary value [really??]

ﬁl

set boundary value from a ﬁle

set to given value(s) or function

nil

do nothing; assume that everything is set

ioc

inlet/outlet on western/eastern hemisphere in cylindrical coordinates

do nothing; assume that everything is set

implies f′(yN) = f′′′(y0) = 0

K.11.2 Boundary condition

bcy

Variable Meaning

Module ‘boundcond.f90’

sds

symmetric-derivative-set

zero value in ghost zones, free value on boundary

periodic

periodic across the pole

Yin-Yang grid

anti-periodic across the pole

symmetry symmetry, fN+i=fN−i;

symmetry with respect to interface

symmetry, plus function value given

sds

symmetric-derivative-set

cds

complex symmetric-derivative-set

s0d

symmetry, function value such that df/dy=0

antisymmetry

248 THE PENCIL CODE

antisymmetry with respect to interface

antisymmetry relative to boundary value

vanishing third derivative

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

onesided

d1s

onesided for 1st and 2nd derivative in two ﬁrst inner points, Dirichlet

in boundary point

n1s

onesided for 1st and 2nd derivative in two ﬁrst inner points, Neumann

in boundary point

constant temp.

symmetric temp.

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

freeze value

s+f

freeze value

“freeze” value, i.e. maintain initial

fBs

frozen-in B-ﬁeld (s)

frozen-in B-ﬁeld (a2)

f=1 (for debugging)

set

set boundary value

sse

symmetry, set boundary value

sep

set boundary value

extrapolation

extrapolation in log [maintain a power law]

der

set derivative on the boundary

cop

outﬂow: copy value of last physical point to all ghost cells

c+k

no-inﬂow: copy value of last physical point to all ghost cells, but sup-

pressing any inﬂow

sfr

stress-free boundary condition for spherical coordinate system.

nfr

Normal-ﬁeld bc for spherical coordinate system. Some people call this

the “(angry) hedgehog bc”.

spt

spherical perfect conducting boundary condition along θboundary f′′ +

cot θf′= 0 and f(xN) = 0

pfc

perfect conducting boundary condition along θboundary

nil’,’

do nothing; assume that everything is set

sep

set boundary value

crk

no-inﬂow: copy value of last physical point to all ghost cells, but sup-

pressing any inﬂow

Module ‘boundcond_alt.f90’

sds

symmetric-derivative-set

zero value in ghost zones, free value on boundary

periodic

periodic across the pole

anti-periodic across the pole

symmetry symmetry, fN+i=fN−i;

symmetry, plus function value given

K.11 Boundary conditions 249

sds

symmetric-derivative-set

cds

complex symmetric-derivative-set

s0d

symmetry, function value such that df/dy=0

antisymmetry

antisymmetry relative to boundary value

vanishing third derivative

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

onesided

constant temp.

symmetric temp.

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

freeze value

s+f

freeze value

“freeze” value, i.e. maintain initial

f=1 (for debugging)

set

set boundary value

sse

symmetry, set boundary value

sep

set boundary value

extrapolation

extrapolation in log [maintain a power law]

der

set derivative on the boundary

cop

outﬂow: copy value of last physical point to all ghost cells

c+k

no-inﬂow: copy value of last physical point to all ghost cells, but sup-

pressing any inﬂow

sfr

stress-free boundary condition for spherical coordinate system.

nfr

Normal-ﬁeld bc for spherical coordinate system. Some people call this

the “(angry) hedgehog bc”.

spt

spherical perfect conducting boundary condition along θboundary f′′ +

cot θf′= 0 and f(xN) = 0

pfc

perfect conducting boundary condition along θboundary

nil’,’

do nothing; assume that everything is set

sep

set boundary value

K.11.3 Boundary condition

bcz

Variable Meaning

Module ‘boundcond.f90’

zero value in ghost zones, free value on boundary

periodic

Yin-Yang grid

symmetry

symmetry with respect to interface

s0d

symmetry, function value such that df/dz=0

0ds

symmetry, function value such that df/dz=0

antisymmetry

250 THE PENCIL CODE

antisymmetry relative to boundary value

a2v

set boundary value and antisymmetry relative to it

antisymmetry with respect to interface

a0d

antisymmetry with zero derivative

vanishing third derivative

one-sided

d1s

onesided for 1st and 2nd derivative in two ﬁrst inner points, Dirichlet

in boundary point

n1s

onesided for 1st and 2nd derivative in two ﬁrst inner points, Neumann

in boundary point

a1s

special for perfect conductor with const alpha and etaT when A con-

sidered as B; one-sided for 1st and 2nd derivative in two ﬁrst inner

points

“freeze” value, i.e. maintain initial

complex

c1s

complex

Fgs

Fconv = - chi t*rho*T*grad(s)

Fct

Fbot = - K*grad(T) - chi t*rho*T*grad(s)

constant ﬂux at the bottom with a variable hcond

pfe

potential ﬁeld extrapolation

p1D

potential ﬁeld extrapolation in 1D

pot

potential magnetic ﬁeld

pwd

a variant of ’pot’ for nprocx=1

hds

hydrostatic equilibrium with a high-frequency ﬁlter

constant temp.

cT1

constant temp.

cT2

constant temp. (keep lnrho)

cT3

constant temp. (keep lnrho)

hydrostatic equilibrium

hse

hydrostatic extrapolation rho or lnrho is extrapolated linearily and the

temperature is calculated in hydrostatic equilibrium.

constant pressure

symmetric temp.

ctz

for interstellar runs copy T

cdz

for interstellar runs limit rho

ism

for interstellar runs limit rho

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

complex

extrapolation

simple linear extrapolation in ﬁrst order

exf

simple linear extrapolation in ﬁrst order

exd

simple linear extrapolation in ﬁrst order

exm

simple linear extrapolation in ﬁrst order

extrapolation with zero value (improved ’a’)

K.11 Boundary conditions 251

extrapolation with zero value (improved ’a’)

f’,’fa

freeze value + antisymmetry

freeze value + symmetry

fBs

frozen-in B-ﬁeld (s)

frozen-in B-ﬁeld (a2)

set to given value(s) or function

f=1 (for debugging)

StS

solar surface boundary conditions

set

set boundary value

der

set derivative on the boundary

div

set the divergence of uto a given value use bc = ’div’ for iuz

ovr

set boundary value

inf

allow inﬂow, but no outﬂow

ouf

allow outﬂow, but no inﬂow

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

in0

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards relaxes to vanishing 1st derivative at boundary

ou0

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards relaxes to vanishing 1st derivative at boundary

ind

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards creates inwards pointing or zero 1st derivative at boundary

oud

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards creates outwards pointing or zero 1st derivative at boundary

ubs

copy boundary outﬂow,

win

forces massﬂux given as Σρi(ui+u0) = fbcz1/2(ρ)

cop

copy value of last physical point to all ghost cells

nil

do nothing; assume that everything is set

Module ‘boundcond_alt.f90’

cfb

radial centrifugal balance

fBs

frozen-in B-ﬁeld (s)

frozen-in B-ﬁeld (a2)

zero value in ghost zones, free value on boundary

periodic

symmetry

symmetry with respect to interface

s0d

symmetry, function value such that df/dz=0

0ds

symmetry, function value such that df/dz=0

antisymmetry

antisymmetry relative to boundary value

antisymmetry with respect to interface

a0d

antisymmetry with zero derivative

vanishing third derivative

one-sided

“freeze” value, i.e. maintain initial

complex

252 THE PENCIL CODE

Fgs

Fconv = - chi t*rho*T*grad(s)

Fct

Fbot = - K*grad(T) - chi t*rho*T*grad(s)

constant ﬂux at the bottom with a variable hcond

pfe

potential ﬁeld extrapolation

p1D

potential ﬁeld extrapolation in 1D

pot

potential magnetic ﬁeld

pwd

a variant of ’pot’ for nprocx=1

hds

hydrostatic equilibrium with a high-frequency ﬁlter

constant temp.

cT2

constant temp. (keep lnrho)

cT3

constant temp. (keep lnrho)

hydrostatic equilibrium

hse

hydrostatic extrapolation rho or lnrho is extrapolated linearily and the

temperature is calculated in hydrostatic equilibrium.

constant pressure

symmetric temp.

ctz

for interstellar runs copy T

cdz

for interstellar runs limit rho

asT

select entropy for uniform ghost temperature matching ﬂuctuating

boundary value, TN−i=TN=; implies T′(xN) = T′(x0) = 0

complex

extrapolation

simple linear extrapolation in ﬁrst order

exf

simple linear extrapolation in ﬁrst order

exd

simple linear extrapolation in ﬁrst order

exm

simple linear extrapolation in ﬁrst order

extrapolation with zero value (improved ’a’)

f’,’fa

freeze value + antisymmetry

freeze value + symmetry

fBs

frozen-in B-ﬁeld (s)

frozen-in B-ﬁeld (a2)

set to given value(s) or function

f=1 (for debugging)

StS

solar surface boundary conditions

set

set boundary value

der

set derivative on the boundary

div

set the divergence of uto a given value use bc = ’div’ for iuz

ovr

set boundary value

inf

allow inﬂow, but no outﬂow

ouf

allow outﬂow, but no inﬂow

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards

out

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards

K.12 Initial condition parameter dependence 253

in0

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards relaxes to vanishing 1st derivative at boundary

ou0

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards relaxes to vanishing 1st derivative at boundary

ind

allow inﬂow, but no outﬂow forces ghost cells and boundary to not point

outwards creates inwards pointing or zero 1st derivative at boundary

oud

allow outﬂow, but no inﬂow forces ghost cells and boundary to not point

inwards creates outwards pointing or zero 1st derivative at boundary

ubs

copy boundary outﬂow,

win

forces massﬂux given as Σρi(ui+u0) = fbcz1/2(ρ)

cop

copy value of last physical point to all ghost cells

nil

do nothing; assume that everything is set

K.12 Initial condition parameter dependence

The following tables list which parameters from each Namelist are required (•), optional

(⋄) or irrelevant (blank). The distinction is made between required and optional where by

a parameter requires a setting if the default value would give an invalid or degenerate

case for the initial condition.

254 THE PENCIL CODE

inituu

ampluu

widthuu

urand

uu left

uu right

uu upper

uu lower

uy left

uy right

kx uu

ky uu

kz uu

zero

gaussian-noise •

gaussian-noise-x •

xjump ⋄ • • • •

Beltrami-x •

Beltrami-y •

Beltrami-z •

trilinear-x •

trilinear-y •

trilinear-z •

cos-cos-sin-uz •

tor pert •

trilinear-x •

sound-wave • •

shock-tube ⋄ • •

bullets • ⋄

Alfven-circ-x • ⋄

const-ux •

const-uy •

tang-discont-z ⋄ • • •

Fourier-trunc • ⋄ • •

up-down • ⋄

initss

ampl ss

radius ss

widthss

epsilon ss

grads0

pertss

ss left

ss right

ss const

mpoly0

mpoly1

mpoly2

isothtop

khor ss

center1 x

center1 y

center1 z

center2 x

center2 y

center2 z

thermal background

thermal peak

zero

const ss •

blob • •

isothermal

K.12 Initial condition parameter dependence 255

Ferri`

ere

xjump • • •

hor-ﬂuxtube • • •

hor-tube • • •

sedov • • • • •

sedov-dual • • • • • • • •

isobaric

isentropic

linprof

piecew-poly

polytropic

256 THE PENCIL CODE

References

[1] Abramowitz, A., Stegun, I. A., Pocketbook of Mathematical Functions, Harri

Deutsch, Frankfurt (1984)

[2] Babkovskaia, N., Haugen, N. E. L., Brandenburg, A.: 2011, “A high-order public

domain code for direct numerical simulations of turbulent combustion,” J. Comp.

Phys. 230, 1-12 (arXiv/1005.5301)

[3] Barekat, A., & Brandenburg, A., Astron. Astrophys. 571, A68 (2014) “Near-

polytropic stellar simulations with a radiative surface”

[4] Brandenburg, A., Astrophys. J. 550, 824–840 (2001) “The inverse cascade and non-

linear alpha-effect in simulations of isotropic helical hydromagnetic turbulence”

[5] Brandenburg, A., in Advances in non-linear dynamos, ed. A. Ferriz-Mas &

M. N ´

u˜

nez Jim´

enez, (The Fluid Mechanics of Astrophysics and Geophysics,

Vol. 9) Taylor & Francis, London and New York, pp. 269–344 (2003);

http://arXiv.org/abs/astro-ph/0109497

[6] Brandenburg, A., Dobler, W., Astron. Astrophys. 369, 329–338 (2001) “Large scale

dynamos with helicity loss through boundaries”

[7] Brandenburg, A., & Hazlehurst, J., Astron. Astrophys. 370, 1092–1102 (2001) “Evo-

lution of highly buoyant thermals in a stratiﬁed layer”

[8] Brandenburg, A., & Sarson, G. R., Phys. Rev. Lett. 88, 055003 (2002) “The effect of

hyperdiffusivity on turbulent dynamos with helicity”

[9] Brandenburg, A., Dobler, W., & Subramanian, K., Astron. Nachr. 323, 99–122

(2002) “Magnetic helicity in stellar dynamos: new numerical experiments”

[10] Brandenburg, A., Enqvist, K., & Olesen, P., Phys. Rev. D 54, 1291–1300 (1996)

“Large-scale magnetic ﬁelds from hydromagnetic turbulence in the very early uni-

verse”

[11] Brandenburg, A., Jennings, R. L., Nordlund, ˚

A., Rieutord, M., Stein, R. F., & Tuomi-

nen, I., J. Fluid Mech. 306, 325–352 (1996) “Magnetic structures in a dynamo sim-

ulation”

[12] A. Brandenburg, T. Kahniashvili, S. Mandal, A. Roper Pol, A. G. Tevzadze, and T.

Vachaspati, Phys. Rev. D 96, 123528 (2017) “Evolution of hydromagnetic turbulence

from the electroweak phase transition”

[13] Brandenburg, A., Moss, D., & Shukurov, A., MNRAS 276, 651–662 (1995) “Galactic

fountains as magnetic pumps”

[14] Brandenburg, A., Nordlund, ˚

A., Stein, R. F., & Torkelsson, U., Astrophys. J. 446,

741–754 (1995) “Dynamo-generated turbulence and large scale magnetic ﬁelds in a

Keplerian shear ﬂow”

[15] Collatz, L., The numerical treatment of differential equations, Springer-Verlag, New

York, p. 164 (1966)

[16] Dobler, W., Stix, M., & Brandenburg, A.: 2006, “Convection and magnetic ﬁeld gen-

eration in fully convective spheres,” Astrophys. J. 638, 336-347

REFERENCES 257

[17] Durrer, R., “The Cosmic Microwave Background,” Cambridge University Press

(2008)

[18] Gammie, C. F., Astrophys. J. 553, 174–183 (2001) “Nonlinear outcome of gravita-

tional instability in cooling, gaseous disks”

[19] Goodman, J., Narayan, R. & Goldreich, P., Month. Not. Roy. Soc. 225, 695–711

(1987) “The stability of accretion tori – II. Nonlinear evolution to discrete planets”

[20] Haugen, N. E. L., & Brandenburg, A. Phys. Rev. E 70, 026405 (2004) “Inertial range

scaling in numerical turbulence with hyperviscosity”

[21] Hockney, R. W., & Eastwood, J. W., Computer Simulation Using Particles, McGraw-

Hill, New York (1981)

[22] Hurlburt, N. E., Toomre, J., & Massaguer, J. M., Astrophys. J. 282, 557–573 (1984)

“Two-dimensional compressible convection extending over multiple scale heights”

[23] Kim, J., Moin, P. & Moser, R J. of Fluid Mech. 177, 133 (1987) “Turbulence statistics

in fully developed channel ﬂow at low Reynolds number”

[24] Kippenhahn, R. & Weigert, A. Stellar structure and evolution, Springer: Berlin

(1990)

[25] Krause, F., R ¨

adler, K.-H., Mean-Field Magnetohydrodynamics and Dynamo Theory,

Akademie-Verlag, Berlin; also Pergamon Press, Oxford (1980)

[26] Lele, S. K., J. Comp. Phys. 103, 16–42 (1992) “Compact ﬁnite difference schemes

with spectral-like resolution”

[27] Misner, C. W., Thorne, K. S. & Wheeler, J. A. Gravitation, San Francisco: W.H.

Freeman and Co. (1973), p. 213.

[28] Mitra, D., Tavakol, R., Brandenburg, A., & Moss, D.: 2009, “Turbulent dynamos in

spherical shell segments of varying geometrical extent,” Astrophys. J. 697, 923-933

(arXiv/0812.3106)

[29] Nordlund, ˚

A., & Galsgaard, K., A 3D MHD code for Parallel Computers,

http://www.astro.ku.dk/~aake/NumericalAstro/papers/kg/mhd.ps.gz (1995)

[30] Nordlund, ˚

A., Stein, R. F., Comput. Phys. Commun. 59, 119 (1990) “3-D simulations

of solar and stellar convection and magnetoconvection”

[31] Press, W., Teukolsky, S., Vetterling, W., & Flannery, B., Numerical Recipes in For-

tran 90, 2nd ed., Cambridge (1996)

[32] Stanescu, D., Habashi, W. G., J. Comp. Phys. 143, 674 (1988) “2N-storage low dissi-

pation and dispersion Runge–Kutta schemes for computational acoustics”

[33] Williamson, J. H., J. Comp. Phys. 35, 48 (1980) “Low-storage Runge–Kutta

schemes”

258 THE PENCIL CODE

259

Part IV

Indexes

File Index

*.c ..........................12

*.f90 ........................12

*.in ..................... 32,181

*.local ......................32

../32c ......................147

.adapt-mkfile.inc ..............78

.bashrc .......................5

.conf ........................19

.cshrc ........................5

.emacs ......................127

.svn/ ........................12

/scratch/ ......................7

<ID> .........................17

$PENCIL_HOME ..................88

$PENCIL_HOME/python ............46

~/.idl_history ................44

~/pencil-auto-test ............108

1D_loop.f90 ..................196

1d-test/ambipolar-diffusion .....66

2d-tests/baroclinic ...........107

2d-tests/battery_term ..........86

2d-tests/spherical_viscous_ring . 107

aa[xyz].{xz,yz,xy,xy2}.........227

ab[xyz].{xz,yz,xy,xy2}.........228

adapt-mkfile ..................22

advective_gauge.f90 ...........196

alive.info ................ 26,183

anelastic.f90 ............ 197,229

auto-test ....................2,9

b2.{xz,yz,xy,xy2}.............227

bb.net .......................42

bb[xyz].{xz,yz,xy,xy2}.........227

beta1.{xz,yz,xy,xy2}..........227

bfield.f90 . . . . . . . . . . . 197, 233, 238

bin/ . . . . . . . . . . 6, 9, 12, 14, 31, 33, 79

boundcond.f90 . . . . . . . . 244, 247, 249

boundcond_alt.f90 . . . . . 246, 248, 251

bugs/ ........................12

cdata.f90 . . . . . . . . . . 90, 110, 188, 228

chem.inp ......................66

chemistry.f90 ................198

chemistry_simple.f90 ..........198

chiral_mhd.f90 ...............198

compilers .....................17

config .................... 18,19

config-local ..................18

config/ ......................18

ConfigFinder ............... 17,18

configure .....................89

conv-slab/ . . . . . . . . . 6, 9, 49, 151, 152

conv-slab/src/ ................11

coronae.f90 ..................199

cosmicray.f90 ................228

cosmicray_current.f90 .........199

cparam.inc .............. 14,32,79

cparam.local . . 6, 12, 14, 22, 41, 49, 54,

102, 147

cparam_pencils.inc ............104

ctimeavg.local . . . . . . . . . . 12, 30, 31

data/ . . . . . . . . . . . 7, 14, 27, 33, 50, 87

data/ .......................15

data/dim.dat .................175

data/param.nml . . . . . . . . 87, 148, 175

data/procN/..................25

data/proc*/ ................ 27,28

datadir.in ............... 7,14,15

debug_c.c ....................111

density.f90 . . 31, 66, 97, 191, 227, 228,

231, 236, 237, 239, 242

density_stratified.f90 . 199, 233, 236,

238, 240, 243

detonate.f90 .................199

developers.txt ..............3,93

dim.dat ................ 15,16,32

divu.{xz,yz,xy,xy2}...........227

doc/ .........................12

dust-vortex/ ..................71

dustdensity.f90 ...............199

dx/ ..........................12

dx/basic ......................41

dx/macros/ ....................32

ec.{xz,yz,xy,xy2}.............228

entropy.f90 31, 111, 191, 227, 228, 231,

236, 237, 240, 242

entropy_anelastic.f90 . . . . . 199, 229

eos_ionization.f90 ............227

Equ ..........................97

equ.f90 .....................100

260

FILE INDEX 261

examples/pro/ .................42

experimental .................128

forced/ ......................12

forced/idl/ ...................55

fourier_fftpack.f90 ............53

fourier_transform_y ............53

generate_kvectors.pro .........151

getconf.csh . . . . . . . . . . . 9, 12, 14, 33

gravitational_waves.f90 ........200

gravitational_waves_hij6.f90 . . . 200

gravitational_waves_hTXk.f90 . . . 200

gravity_simple.f90 201, 233, 236, 238,

243

gravz/ .......................12

grid.dat ................... 16,23

H2_flamespeed/ ................38

heatflux.f90 .................201

helical-MHDturb ...............151

helical-MHDturb/ ...............35

host-ID ......................18

host_ID.conf ..................17

hosts .................... 17,108

hosts/ .......................18

hsections.pro ................152

hydro.f90 . . . . . 31, 66, 77, 97, 102, 188,

227–229, 236, 237, 239, 241

hyperresi_strict_2nd ..........139

hypervisc_strict_2nd ..........139

idl/ ...................... 12,43

index.pro .................. 15,32

inlinedoc-modules.tex .........173

Intel.conf ....................17

Intel_MPI.conf ................17

interlocked-fluxrings .........107

interstellar.dat ...............15

Isurf.xz .....................227

j2.{xz,yz,xy,xy2}.............227

jb.{xz,yz,xy,xy2}.............227

jj[xyz].{xz,yz,xy,xy2}. . . . . . . . . 227

k.dat .................... 32,151

K_VECTORS/ ...................151

kinematic/ ....................12

legend.dat ....................15

lncc.{xz,yz,xy,xy2}...........228

lnrho.{xz,yz,xy,xy2}..........227

lnrho.net .....................42

lnTT.{xz,yz,xy,xy2}...........227

lorenz_gauge.f90 ..............201

mach.{xz,yz,xy,xy2}...........227

magnetic.f90 viii, 31, 98, 100, 101, 111,

192, 227, 228, 231, 236, 238, 240,

243

magnetic_shearboxJ.f90 . 202, 229, 233,

236, 238, 240, 243

Makefile . 13, 21, 22, 31, 32, 79, 80, 124

Makefile.local viii, 6, 12–14, 32, 49, 52,

54, 62, 64, 78, 79, 89

Makefile.src . . . . . . . . 6, 12, 14, 21, 79

manual.tex ................ 91,106

meanfield.f90 . . . . . . . . 206, 235, 241

meanfield_demfdt.f90 ..........206

mkcparam ............... 14,79,104

mpicomm.f90 ...................80

neutraldensity.f90 .............66

neutralvelocity.f90 ............66

NEWDIR .................... 34,84

nochiral ......................79

noentropy.f90 ................206

NOERASE ......................87

noinitial_condition.f90 ........106

noionization.f90 ..............184

nomagnetic.f90 . . . . . . . . viii, 100, 101

nompicomm.f90 ............. 80,113

nospecial.f90 ................105

o2.{xz,yz,xy,xy2}.............227

oo[xyz].{xz,yz,xy,xy2}.........227

os/Unix.conf ..................19

param.nml .............. 15,32,147

param2.nml ................. 15,32

params.log .............. 15,33,34

particles_caustics.f90 .........206

particles_chemistry.f90 ........206

particles_dust.f90 ............206

particles_dust_brdeplete.f90 . . . 207

particles_lagrangian.f90 .......207

particles_mass_swarm.f90 .......207

particles_surfspec.f90 .........207

pc_read_phiavg.pro .............30

pc_read_video .................28

pc_read_xyaver ................29

pc_setupsrc ....................6

pencil-code/ ............ 11,12,88

pencil-code/idl/read ............8

pencil-code/utils ..............33

262 THE PENCIL CODE

pencil-runs/ ..................12

Pencil::ConfigFinder ...........17

Pencil::ConfigParser ...........17

pencil_check.f90 ...............83

phiaver.in ................ 29,228

phiaverages.dat ................29

PHIAVGN......................30

phiavg.pro ....................30

polymer.f90 ..................207

power ........................53

power.pro .....................54

power_kin.dat .................52

power_krms.dat ................53

powerbx_x.dat .................52

powerhel_mag.dat ...............52

powerux_x.dat .............. 52,53

Poynting[xyz].{xz,yz,xy,xy2}. . . . 227

pp.{xz,yz,xy,xy2}.............227

print.in . . 8, 14, 25, 100, 101, 148, 188

procN.................. 15,32,33

proc0 ........................15

proc1 ........................15

procN/ ......................110

pscalar.f90 .............. 196,228

Qrad.{xz,yz,xy,xy2}...........227

r.pro .................. 44,45,50

r75612.f90 ...................207

r75759.f90 ...................208

radiation_ray.f90 .............227

rall.pro ................ 44,45,50

README . . . . . . . . . . . . . . . 32, 109, 151

reference.out ...............8,14

RELOAD ................. 15,33,34

remesh.csh ...................174

RERUN ..................... 34,84

rho.{xz,yz,xy,xy2}............227

rings/ .......................12

run.csh . . . . . . 9, 12, 14, 31, 33, 34, 84

run.in . . . . . . . . . . . . viii, 8, 14, 26–28,

30–32, 34, 37–40, 52, 54, 83, 102,

147, 154, 181

run.pro ......................32

run.x . . . . . . . . . . . . . 8, 15, 31, 39, 109

runA_32a ......................22

runs/ ........................12

rvid_box ......................27

rvid_box.pro ..................27

rvid_line.pro .................27

rvid_plane.pro ................27

samples/ . . . . . . . . . . . 2, 3, 5, 9, 14, 121

samples/parameter_scan ..........32

samples/README ................12

SCRATCH_DIR ...................84

sedimentation/ ................56

seed.dat ................... 16,40

sfb-1.dat .....................54

sfu-1.dat .....................54

sfz1-1.dat ....................54

shear.f90 ....................209

shock.{xz,yz,xy,xy2}..........227

shock.f90 ................ 209,227

shock_highorder.f90 209, 235, 236, 239

slice ........................87

slice_uu1.yz ..................27

slize* .......................27

solar_corona.f90 ..............209

solid_cells_CGEO.f90 ..........209

solid_cells_ogrid_chemistry.f90 . 209

solid_cells_reactive.f90 .......209

sound-spherical-noequi/ .........24

sourceme ....................5,76

sourceme.csh . . . . . . . . . . 5, 12, 76, 87

sourceme.sh . . . . . . . . . . . 5, 12, 76, 87

SPEED ........................33

spher/ .......................12

src/ . . . . . . . viii, 3, 6, 11, 12, 14, 33, 79

src/ ........................14

src/*.local ...................32

src/cparam.local ..............147

src/Makefile.inc ...............52

src/Makefile.local . . 38, 106, 147, 153

src/read_all_videofiles.x .......27

src/read_videofiles.x . . . . . . . 27, 28

ss.{xz,yz,xy,xy2}.............227

ss.net .......................42

start.csh . . 9, 12, 14, 31, 33, 39, 67, 83

start.inviii, 8, 14, 24, 28, 32, 34, 35, 37,

39, 41, 59, 83, 102, 106, 148, 154,

174, 181

start.pro ............... 32,44,87

start.x . 8, 15, 39, 41, 78, 83, 109, 185

STOP ...................... 33,34

structure.pro .................55

sub.f90 ......................98

TAVGN........................31

temperature_idealgas.f90 . . . 209, 227,

235, 236, 239, 241, 244

temperature_ionization.f90 . 210, 235

test_chemistry.f90 ............210

FILE INDEX 263

testfield_axisym.f90 ..........210

testfield_axisym2.f90 .........211

testfield_axisym4.f90 .........211

testfield_compress_z.f90 .......212

testfield_meri.f90 ............214

testfield_nonlin_z.f90 . . . . . . . . . 215

testfield_x.f90 ...............217

testfield_xz.f90 ..............219

testfield_z.f90 ...............219

testflow_z.f90 ...............221

testperturb.f90 ...............221

testscalar.f90 ...............222

testscalar_axisym.f90 .........223

testscalar_simple.f90 .........224

thermal_energy.f90 226, 235, 237, 239,

241, 244

time.dat ................... 16,40

time_series.dat 8, 14, 15, 25, 32, 33, 41,

timeavg.dat ...................31

top.log ......................33

tran.dat ......................66

ts.pro ................ 42,44,152

tsnap.dat ................. 15,182

TT.{xz,yz,xy,xy2}.............227

tvid.dat ......................15

u2.{xz,yz,xy,xy2}.............227

u[xyz].{xz,yz,xy,xy2}..........227

uu.net .......................42

VAR ................... 40,87,183

VARN. . . . . . 15, 16, 26, 32, 33, 36, 182

var.dat 8, 15, 16, 25, 31, 32, 34, 36, 40,

42, 45, 87, 146, 174, 182, 183

var.general ...................41

VAR0 ........................174

VAR1 ........................146

VAR# .........................34

video.in . . . . . . . . . . . . 26–28, 148, 227

visc_smagorinsky.f90 ..........226

viscosity.f90 . . . . . 226, 235, 239, 244

vsections.pro ................153

vsections2.pro ...............153

X.xy .........................16

X.xz .........................16

X.yz .........................16

xyaver.in ............. 29,148,229

xyaverages.dat ................29

xzaver.in ............. 29,235,236

xzaverages.dat ................29

yaver.in .................. 29,239

yaverages.dat .................29

yH.{xz,yz,xy,xy2}.............227

yzaver.in ................. 29,237

yzaverages.dat ................29

zaver.in .................. 29,241

zaverages.dat .................29

Variable Index

.true. .........................29

0ds ..................... 249,251

1s . . . . . . . . . . . . . . . 245, 246, 248–251

1so ..................... 245,246

0. . . . . . . . . . . . . . . . 244, 246–249, 251

1. . . . . . . . . . . . 245, 247–249, 251, 252

a. . . . . . . . . . . . 244, 246, 247, 249, 251

a0d ..................... 250,251

a11xy .......................214

a12xy .......................214

a13xy .......................214

a1s .........................250

a2 . . . . . . . . . . . . . . . 245, 246, 248–251

a21xy .......................214

a22xy .......................214

a23xy .......................214

a2m .................... 194,204

a2r ..................... 245,246

a2v ..................... 245,250

a31xy .......................214

a32xy .......................214

a33xy .......................214

aa ..........................227

ab ..........................228

ab int ................... 192,202

ABC A......................186

ABC B......................186

ABC C......................186

abm .................... 192,202

abmh ................... 192,202

abmn ................... 192,202

abms ................... 192,202

abmxy .................. 243,244

abmz ................... 232,234

abrms ................... 192,202

abumx .................. 192,202

abumy .................. 192,202

abumz .................. 192,202

abuxmz .................. 232,233

abuymz .................. 232,233

abuzmz .................. 232,233

accpowzdownmz ...............231

accpowzmz ...................231

accpowzupmz .................231

af . . . . . . . . . . . . . . . 244, 248, 250, 251

ajm ..................... 192,202

aklam .......................221

aklamQ .....................221

alp11 . . . . . . . . 212, 215, 217, 219, 222

alp11 x......................217

alp11 x2 .....................218

alp11cc . . . . . . . . . . . 212, 215, 217, 219

alp11x ......................218

alp11z ......................220

alp12 . . . . . . . . 212, 215, 217, 219, 222

alp12 x......................218

alp12 x2 .....................218

alp12cs . . . . . . . . . . . 212, 215, 217, 219

alp12x ......................218

alp12z ......................220

alp13 .......................219

alp13z ......................220

alp21 . . . . . . . . 212, 215, 217, 219, 222

alp21 x ......................218

alp21 x2 .....................218

alp21sc . . . . . . . . . . . 212, 215, 217, 219

alp21x ......................218

alp21z ......................220

alp22 . . . . . . . . 212, 215, 217, 219, 222

alp22 x......................218

alp22 x2 .....................218

alp22ss . . . . . . . . . . . 212, 215, 217, 219

alp22x ......................218

alp22z ......................220

alp23 .......................219

alp23z ......................220

alp31 . . . . . . . . 212, 215, 217, 219, 222

alp32 . . . . . . . . 212, 215, 217, 219, 222

alpK .................... 212,215

alpM ................... 212,215

alpm ........................206

alpMK .................. 212,215

alpmxz ......................241

alpPARA ................ 210,211

alpPARAz ................ 210,211

alpPERP ................ 210,211

alpPERPz ................ 210,211

amax ................... 194,204

ambmz .................. 195,204

ambmzh ................. 195,205

264

VARIABLE INDEX 265

ambmzn ................. 195,205

ambmzs ................. 195,205

ampl ff ......................187

ampl forc ....................184

ampl ss .....................178

amplaa ......................180

amplaa2 .....................180

ampllncc ....................180

ampllncc2 ....................180

ampllnrho ...................177

ampluu .................. 130,176

ant ..................... 245,247

ap ...................... 247,248

apbrms ......................197

arms .................... 194,204

asT . . . . . . . . . . 245, 246, 248–250, 252

axmxy .......................243

axmxz .......................240

axmz ................... 232,233

axp2 .................... 193,203

axpt .................... 193,203

aymxy .......................243

aymxz .......................240

aymz ................... 232,233

ayp2 .................... 194,203

aypt .................... 193,203

azmxy .......................243

azmxz .......................240

azmz .................... 232,233

azp2 .................... 194,203

azpt .................... 193,203

b0rms . . . . . . . . . . . . 213, 216, 218, 220

b1 ...................... 250,252

b111xy ......................214

b112xy ......................215

b11rms . . . . . . . . . . . 213, 216, 218–220

b121xy ......................215

b122xy ......................215

b12rms . . . . . . . . . . . 213, 216, 218, 220

b131xy ......................215

b132xy ......................215

b1b23m ................. 195,205

b1b32m ................. 195,205

b1m .................... 192,202

b1rms ................... 210,211

b2 . . . . . . . . . . . . . . . . . . 227, 250, 252

b211xy ......................215

b212xy ......................215

b21rms . . . . . . . . . . . 213, 216, 218–220

b221xy ......................215

b222xy ......................215

b22rms . . . . . . . . . . . 213, 216, 218, 220

b231xy ......................215

b232xy ......................215

b2b13m ................. 195,205

b2b31m ................. 195,205

b2divum ................. 196,205

b2m ................ 192,197,202

b2mphi ......................229

b2mx .......................238

b2mxz .......................240

b2mz ................... 233,235

b2rms .......................211

b2ruzm .................. 192,202

b2tm .................... 192,202

b2uzm .................. 192,202

b3 ...................... 251,252

b311xy ......................215

b312xy ......................215

b321xy ......................215

b322xy ......................215

b331xy ......................215

b332xy ......................215

b3b12m ................. 195,205

b3b21m ................. 195,205

b3rms .......................211

b4m ........................192

Bext ........................186

bamp ............... 213,217,220

bb ...................... 111,227

bbmphi .................. 228,229

bbsphmphi ...................229

bbxmax .................. 194,203

bbxmz ................... 232,234

bbymax .................. 194,203

bbymz ................... 232,234

bbzmax .................. 194,203

bbzmz ................... 232,234

bc{x,y,z}......................39

bcosphz .................. 195,204

bcx . . . . . . . . . 39, 40, 84, 175, 183, 244

bcy . . . . . . . . . . . . . . . 39, 175, 183, 247

bcz . . . . . . . . . 39, 40, 84, 176, 183, 249

beta1 .......................227

beta1m .................. 194,204

beta1max ................ 194,204

beta1mxy ................ 243,244

beta1mz ................. 232,234

beta2mx ................. 238,239

beta2mz ................. 232–234

266 THE PENCIL CODE

betam . . . . . . . . . . . . . . . 194, 198, 204

betamax . . . . . . . . . . . . . 194, 198, 204

betamin . . . . . . . . . . . . . 194, 198, 204

betamx .................. 238,239

betamz .................. 232–234

betPARA ................. 210,211

betPARAz ................ 210,211

betPERP ................. 210,211

betPERP2 ....................211

betPERPz ................ 210,211

bf2m ........................194

bf2mz ................... 233,235

bf4m ........................194

bfrms ................... 194,203

bgmu5rms ...................198

bgmuSrms ...................198

bjtm .................... 192,202

blowupm ....................206

bm .........................197

bm2 .................... 192,202

bmax . . . . . . . . . . . . . . . 194, 197, 203

bmin ........................197

bmx . . . . . . . . . . . . . . 29, 194, 204, 238

bmxy rms ................ 196,205

bmy . . . . . . . . . . . . . . . . . 29, 194, 204

bmz . . . . . . . . . . . . . . 29, 195, 204, 233

bmzA2 .................. 195,204

bmzph .................. 195,204

bmzphe .................. 195,204

bmzS2 .................. 195,204

bpmphi .................. 228,229

brmphi .................. 228,229

brms . . . . . . . . . . . . . 130, 194, 197, 203

brmsx ................... 196,206

brmsz ................... 196,206

brsphmphi ...................229

bsinphz .................. 195,204

bthmphi .....................229

bx0mz . . . . . . . . . . . . 214, 217, 218, 221

bx0pt . . . . . . . . . . . . . . . 212, 216, 220

bx11pt . . . . . . . . . . . . . . 212, 216, 220

bx12pt . . . . . . . . . . . . . . 212, 216, 220

bx1mxz ......................240

bx1pt ................... 210,211

bx21pt . . . . . . . . . . . . . . 212, 216, 220

bx22pt . . . . . . . . . . . . . . 212, 216, 220

bx2m . . . . . . . . . . . . . . . 195, 197, 205

bx2mx .................. 238,239

bx2mxy ......................243

bx2mxz .................. 240,241

bx2my ......................236

bx2mz ................... 232–234

bx2pt ................... 210,211

bx2rmz .................. 232,234

bx3pt ................... 210,211

bxbym . . . . . . . . . . . . . . 194, 197, 204

bxbymx .................. 238,239

bxbymxy ................. 243,244

bxbymxz ................. 240,241

bxbymy ......................236

bxbymz .................. 233,234

bxbzm .......................197

bxbzmx .................. 238,239

bxbzmxy ................. 243,244

bxbzmxz ................. 240,241

bxbzmy ......................236

bxbzmz .................. 233,234

bxm ................ 194,197,204

bxmax . . . . . . . . . . . . . . 194, 197, 203

bxmin ................... 194,203

bxmx ................... 238,239

bxmxy .......................243

bxmxz .......................240

bxmy .......................236

bxmz ................... 232–234

bxp2 .................... 193,203

bxpt .................... 193,203

by0mz . . . . . . . . . . . . 214, 217, 218, 221

by0pt . . . . . . . . . . . . . . . 213, 216, 220

by11pt . . . . . . . . . . . . . . 212, 216, 220

by12pt . . . . . . . . . . . . . . 213, 216, 220

by1mxz ......................240

by21pt . . . . . . . . . . . . . . 212, 216, 220

by22pt . . . . . . . . . . . . . . 213, 216, 220

by2m . . . . . . . . . . . . . . . 195, 197, 205

by2mx .................. 238,239

by2mxy .................. 243,244

by2mxz .................. 240,241

by2my ......................236

by2mz ................... 232–234

by2rmz .................. 232,234

bybzm .......................197

bybzmx .................. 238,239

bybzmxy ................. 243,244

bybzmxz ................. 240,241

bybzmy ......................236

bybzmz .................. 233,234

bym ................ 194,197,204

bymax . . . . . . . . . . . . . . 194, 197, 203

bymin ................... 194,203

VARIABLE INDEX 267

bymx ................... 238,239

bymxy .......................243

bymxz .......................240

bymy .......................236

bymz ................... 232–234

byp2 .................... 193,203

bypt .................... 193,203

bz0mz . . . . . . . . . . . . 214, 217, 218, 221

bz1mxz ......................240

bz2m ............... 195,197,205

bz2mx ................... 238,239

bz2mxy .................. 243,244

bz2mxz .................. 240,241

bz2my .......................236

bz2mz ................... 232–234

bz2rmz .................. 232,234

bzm ................ 194,197,204

bzmax ............... 194,197,203

bzmin ................... 194,203

bzmphi .................. 228,229

bzmx ................... 238,239

bzmxy .......................243

bzmxz .......................240

bzmy .......................236

bzmz .................... 232–234

bzp2 .................... 193,203

bzpt .................... 193,203

c+k ..................... 248,249

c1 . . . . . . . . . . . . . . . 245, 246, 250, 251

c1pt ................ 223,224,226

c1rms ................... 223–225

c1s .........................250

c2 ...................... 250,252

c2pt ................ 223,224,226

c2rms ................... 223–225

c3 ...................... 250,252

c3pt ................ 223,224,226

c3rms ................... 223–225

c4pt ................ 223,224,226

c4rms ................... 223–225

c5pt ................ 223,224,226

c5rms ................... 223–225

c6pt ................ 223,224,226

c6rms ................... 223–225

ccglnrm .....................196

ccmax .......................196

cdiffrho .....................184

cds ..................... 247,249

cdt ................... 38,41,182

cdts .........................38

cdtv ..................... 38,182

cdz ..................... 250,252

ce ...................... 250,252

cfb ..................... 246,251

cgam .......................191

chemistry.f90 .................173

chi .........................185

chi t........................185

CHIRAL ......................79

coeff grid .................. 23,25

cool .........................185

cooltype .....................185

cop . . . . . . 245, 246, 248, 249, 251, 253

cosjbm .................. 196,206

cosubm .................. 193,202

cp ...................... 250,252

cpc ..................... 245,246

cpp ..................... 245,246

cpz ..................... 245,246

crk .........................248

cs0 ..................... 177,184

cs2 .........................111

cs2bot ................... 177,184

cs2cool ......................185

cs2mphi ................. 228,229

cs2top ................... 177,184

csm ................. 191,199,210

csmax ................... 191,210

cT . . . . . . . . . . . 245, 246, 248–250, 252

cT1 .........................250

cT2 ..................... 250,252

cT3 ..................... 250,252

ctz ..................... 250,252

curlru2mz ....................229

cutoff .......................130

cvsid .................... 174,181

d1s ................. 245,248,250

d2davg ................... 30,183

d2Lambrms ..................197

d2Lamrms ...................197

d6abmz ................. 232,234

d6amz1 ................. 232,234

d6amz2 ................. 232,234

d6amz3 ................. 232,234

damp ................... 183,184

dampu ......................183

dampuext ....................183

dampuint ....................183

datadir .......................45

db ...................... 250,252

268 THE PENCIL CODE

dbx2m ......................198

dbxm .......................197

dbxmax .....................197

dby2m ......................198

dbym .......................197

dbymax .....................197

dbz2m ......................198

dbzm .......................198

dbzmax ......................197

dcoolx .......................238

dcoolxy ......................242

dcoolz .......................231

del ..................... 210,211

del2 ........................211

deltay .......................209

delz .................... 210,211

der . . . . . . . . . . 245, 247–249, 251, 252

detn ........................199

dettot .......................199

dexbmx .................. 196,205

dexbmy .................. 196,205

dexbmz .................. 196,205

dheat buffer1 .................185

diffrho hyper3 mesh ............143

div ..................... 251,252

divabrms ....................197

divapbrms ...................197

divarms ................. 194,204

divbmax .....................198

divbrms .....................198

divrhoum ....................197

divrhoumax .............. 190,197

divrhourms .............. 190,197

divru2mz ....................229

divu ........................227

divu2m ......................189

divu2mz .....................229

divuHrms ....................191

divum .......................189

divumz ......................229

dobrms .................. 193,202

dr0 ..................... 245,247

drho2m ................. 191,199

drho2mx .....................238

drho2mxy ....................243

drho2mxz ....................240

drho2my .....................236

drho2mz .....................233

drhom .................. 191,199

drhomax .....................199

drhomx ......................238

drhomxy .....................243

drhomxz .....................240

drhomy ......................236

drhomz ......................233

drhorms .....................199

dsnap ................. 26,36,182

dstalk .......................181

dt . . . . . . . . . . . . . . . 8, 38, 41, 182, 188

dt bb 1 ......................199

dt chiral .....................199

dt mu5 1 ....................198

dt mu5 2 ....................198

dt mu5 3 ....................198

dt mu5 4 ....................199

dt muS 1 ....................199

dt muS 2 ....................199

dtb ..................... 194,204

dtc . . . . . . . . . . . . 8, 191, 199, 206, 210

dtchem . . . . . . . . . . . . . . 198, 209, 210

dtchi . . . . . . . . . . . . . . . 8, 191, 200, 210

dtchi2 . . . . . . . . . . . . . . . 196, 199, 209

dteta .................... 194,204

dtF .........................191

dtH ........................192

dtmin .......................182

dtnewt ......................209

dtnu ...................... 8,226

dtpchem .....................207

dtq .........................201

dtq2 ........................201

dtrad ................... 196,199

dtradloss ....................209

dtshear ......................209

dtspitzer . . . . . . . . . . 196, 199, 201, 209

dtu ....................... 8,190

dtvel ........................209

dubrms .................. 193,202

dudx ........................190

durms .......................188

dvid . . . . . . . . . . . . . . . . 26, 27, 36, 182

dz 1.........................23

dz tilde .......................23

E0rms . . . . . . . . . . . 213, 216, 218, 220

E0Um . . . . . . . . . . . . . . . 214, 217, 221

E0Wm . . . . . . . . . . . . . . 214, 217, 221

e1 . . . . . . . . . . . . . . . 245, 247–250, 252

E10z . . . . . . . . . . . . . 213, 217, 218, 221

E111z . . . . . . . . . . . . 213, 217–219, 221

E112z . . . . . . . . . . . . 213, 217, 218, 221

VARIABLE INDEX 269

E11rms . . . . . . . . . . 213, 216, 218, 220

E11xy .......................214

E121z . . . . . . . . . . . . 213, 217–219, 221

E122z . . . . . . . . . . . . 213, 217, 218, 221

E12rms . . . . . . . . . . 213, 216, 218, 220

E12xy .......................214

E13xy .......................214

e1o ..................... 245,247

e2 . . . . . . . . . . . . . . . 245, 247–250, 252

E20z . . . . . . . . . . . . . 214, 217, 218, 221

E211z . . . . . . . . . . . . 213, 217–219, 221

E212z . . . . . . . . . . . . 213, 217, 218, 221

E21rms . . . . . . . . . . 213, 216, 218, 220

E21xy .......................214

E221z . . . . . . . . . . . . 213, 217–219, 221

E222z . . . . . . . . . . . . 213, 217, 218, 221

E22rms . . . . . . . . . . 213, 216, 218, 220

E22xy .......................214

E23xy .......................214

e3 . . . . . . . . . . . . . . . . . . 245, 247–249

E30z . . . . . . . . . . . . . 214, 217, 218, 221

E311z . . . . . . . . . . . . 213, 217–219, 221

E312z . . . . . . . . . . . . 213, 217, 218, 221

E31xy .......................214

E321z . . . . . . . . . . . . 213, 217–219, 221

E322z . . . . . . . . . . . . 213, 217, 218, 221

E32xy .......................214

E33xy .......................214

e3xamz1 ................. 233,234

e3xamz2 ................. 233,234

e3xamz3 ................. 233,234

E41xy .......................214

E42xy .......................214

E43xy .......................214

E51xy .......................214

E52xy .......................214

E53xy .......................214

E61xy .......................214

E62xy .......................214

E63xy .......................214

E71xy .......................214

E72xy .......................214

E73xy .......................214

E81xy .......................214

E82xy .......................214

E83xy .......................214

E91xy .......................214

E92xy .......................214

E93xy .......................214

EBpq . . . . . . . . . . . . 214, 217, 218, 221

ecr .........................228

EEGW .................. 200,201

EEM .......................192

eem . . . . . . . . . . . . . . 191, 199, 210, 226

eemz ........................235

ekin ........................190

ekincr .......................199

ekinmx ......................237

ekinmz ......................230

ekinp .......................207

ekintot ......................190

el ..........................245

emag ................... 194,203

embmz .................. 195,204

EMFdotB int .................206

EMFdotBm ..................206

EMFmax ....................206

EMFmin .....................206

EMFmz1 ....................206

EMFmz2 ....................206

EMFmz3 ....................206

EMFrms .....................206

emxamz3 ................ 195,204

Emymxz .....................241

Emzmask ....................210

Emzmxy .....................244

eos merger ....................90

epot ........................201

epotmx ......................238

epotmxy .....................243

epotmy ......................236

epotmz ......................233

epottot ......................201

epotuxmx ....................238

epotuxmxy ...................243

epotuzmz ....................233

epsAD ................... 193,203

epsilonaa ....................180

epsK ........................226

epsKmz ......................235

epsM ................... 193,203

epsMmz ................. 233,235

eruzmz ......................235

eta .........................186

eta11 . . . . . . . . 212, 215, 217, 219, 222

eta11 x......................218

eta11 x2 .....................218

eta11cc . . . . . . . . . . . 212, 215, 217, 219

eta11x .......................219

eta11z .......................220

270 THE PENCIL CODE

eta12 . . . . . . . . 212, 215, 217, 219, 222

eta12 x ......................218

eta12 x2 .....................218

eta12cs . . . . . . . . . . . 212, 216, 217, 219

eta12x .......................219

eta12z .......................220

eta21 . . . . . . . . 212, 215, 217, 219, 222

eta21 x ......................218

eta21 x2 .....................218

eta21sc . . . . . . . . . . . 212, 215, 217, 219

eta21x .......................219

eta21z .......................220

eta22 . . . . . . . . 212, 215, 217, 219, 222

eta22 x ......................218

eta22 x2 .....................218

eta22ss . . . . . . . . . . . 212, 216, 217, 219

eta22x .......................219

eta22z .......................220

eta31 ................... 219,222

eta32 ................... 219,222

eta ext ......................186

eta int ......................186

eta out ......................186

eta tdep .....................192

etaj2max ................ 196,206

etajmax ................. 196,206

etajrhomax ............... 196,206

etasmagm ................ 196,205

etasmagmax .............. 196,205

etasmagmin .............. 196,205

etatm .......................206

etatotalmx ............... 238,239

etatotalmz ............... 233,234

etavamax ................ 196,205

ethm . . . . . . . . . 191, 199, 206, 210, 226

ethmax ......................226

ethmcr ......................199

ethmin ......................226

ethmz ................... 231,235

ethtot . . . . . . . . . . . . 191, 200, 210, 226

etot .........................226

ex ...................... 250,252

Ex0pt . . . . . . . . . . . . . . . 213, 216, 220

Ex11pt . . . . . . . . . . . . . . 213, 216, 220

Ex12pt . . . . . . . . . . . . . . 213, 216, 220

Ex21pt . . . . . . . . . . . . . . 213, 216, 220

Ex22pt . . . . . . . . . . . . . . 213, 216, 220

exabot ................... 194,203

examx ................... 196,205

examxy1 ................. 243,244

examxy2 ................. 243,244

examxy3 ................. 243,244

examy ................... 196,205

examz ................... 196,205

examz1 .................. 232,234

examz2 .................. 233,234

examz3 .................. 233,234

exatop ................... 194,203

exd ..................... 250,252

exf ..................... 250,252

exjmx ................... 196,205

exjmy ................... 196,205

exjmz ................... 196,205

exm .................... 250,252

Exmxy .................. 196,206

Exmxz .................. 240,241

Exmz ................... 232,234

Exp2 .................... 193,203

Expt .................... 193,203

Ey0pt . . . . . . . . . . . . . . . 213, 217, 220

Ey11pt . . . . . . . . . . . . . . 213, 216, 220

Ey12pt . . . . . . . . . . . . . . 213, 217, 220

Ey21pt . . . . . . . . . . . . . . 213, 217, 220

Ey22pt . . . . . . . . . . . . . . 213, 217, 220

Eymxy .................. 196,206

Eymxz .................. 240,241

Eymz ................... 232,234

Eyp2 .................... 193,203

Eypt .................... 193,203

Ezmxy .................. 196,206

Ezmxz .................. 240,241

Ezmz ................... 232,234

Ezp2 .................... 193,203

Ezpt .................... 193,203

f................... 245,247–249

f’,’fa .................... 251,252

F11z . . . . . . . . . . . . . . . . 223, 224, 226

F12z . . . . . . . . . . . . . . . . 223, 224, 226

F21z . . . . . . . . . . . . . . . . 223, 224, 226

F22z . . . . . . . . . . . . . . . . 223, 224, 226

F31z . . . . . . . . . . . . . . . . 223, 224, 226

F32z . . . . . . . . . . . . . . . . 223, 224, 226

fB .................. 248,251,252

fbcx ........................245

fbcx12 .......................247

fbcx2 ........................245

fbm ..................... 193,203

Fbot ........................185

fBs ................. 248,251,252

FC ..........................82

VARIABLE INDEX 271

Fcm .................... 245,246

fconvm ......................192

fconvmz .....................235

fconvxmx ....................238

fconvxy ......................242

fconvyxy .....................242

fconvz .......................231

fconvzxy .....................242

Fct . . . . . . . . . . . . . . 245, 246, 250, 252

ffakez .......................235

FFLAGS DOUBLE ..............52

fg . . . . . . . . . . . . . . . . . . 245, 247–251

Fgs . . . . . . . . . . . . . . 245, 246, 250, 252

ﬁl ...................... 246,247

ﬁx ...................... 246,247

fkinxmx .....................231

fkinxmxy ....................242

fkinymxy ....................242

fkinzm ......................188

fkinzmz .....................229

fmasszmz ....................229

fmax ........................100

force ........................187

fountain .....................187

fpresxmz .....................235

fpresymz .....................235

fpreszmz .....................235

fradbot .............. 191,200,209

fradmx ......................238

fradmz ......................235

fradtop .............. 191,200,209

fradx kramers ................238

fradxy Kprof .................242

fradxy kramers ................242

fradymxy Kprof ...............242

fradz .......................231

fradz constchi .................231

fradz Kprof ..................231

fradz kramers .................231

fring1,fring2 ..................180

frmax .......................207

fs ...................... 251,252

fsum ........................100

fturbfz ......................231

fturbmx .....................238

fturbmz .....................231

fturbrxy .....................242

fturbthxy ....................242

fturbtz ......................231

fturbxy ......................242

fturbymxy ....................242

fturbz .......................231

fum ........................190

fviscm .......................226

fviscmax .....................226

fviscmin .....................226

fviscmx ......................239

fviscmxy .....................244

fviscmz ......................235

fviscrmsx ....................226

fviscsmmxy ...................244

fviscsmmz ....................235

fviscymxy ....................244

fxbxm ................... 193,203

g. . . . . . . . . . . . . . . . 246, 247, 251, 252

g11pt ............... 200,207,208

g12pt ............... 200,207,208

g22pt ............... 200,207,208

g23pt ............... 200,201,208

g31pt ............... 200,201,208

g33pt ............... 200,207,208

gal .........................221

gam .................... 210,211

gam11 .............. 222,223,225

gam11z .............. 222,224,225

gam12 .............. 222,223,225

gam12z .............. 222,224,225

gam13 .............. 222,223,225

gam13z .............. 222,224,225

gam21 .............. 222,223,225

gam21z .............. 222,224,225

gam22 .............. 222,223,225

gam22z .............. 222,224,225

gam23 .............. 222,223,225

gam23z .............. 222,224,225

gam31 .............. 222,223,225

gam31z .............. 222,224,225

gam32 .............. 222,223,225

gam32z .............. 222,224,225

gam33 .............. 222,223,225

gam33z .............. 222,224,225

gam3z ......................224

gamc .......................223

gamcz .......................223

gamma . . . . . . . . . . . . . . 177, 184, 221

gammaQ ....................221

gamz ................... 210,211

gdivu2m .....................189

gg2m ............... 200,201,208

ggT2m .............. 200,201,208

272 THE PENCIL CODE

ggTm ................... 201,208

ggTp2 . . . . . . . . . . . . . . . 200, 201, 208

ggTpt . . . . . . . . . . . . . . . 200, 201, 208

ggTXm . . . . . . . . . . . . . . 200, 201, 208

ggX2m . . . . . . . . . . . . . . 200, 201, 208

ggXm ................... 201,208

ggXp2 . . . . . . . . . . . . . . . 200, 201, 208

ggXpt . . . . . . . . . . . . . . . 200, 201, 208

gijij2m ......................201

gLambm .....................197

gLamrms ....................197

gmu5mx .....................198

gmu5my .....................198

gmu5mz .....................198

gmu5rms ....................198

gpu astaroth.f90 ...............173

grads0 ......................178

grav amp ....................178

grav proﬁle . . . . . . . . 131, 132, 177, 187

grav tilt .....................178

gravz . . . . . . . . . . . . . . . 131, 177, 187

grhomax .....................191

grid func .....................23

gshockmax ...................209

gsrms .......................192

gsxmxy ......................242

gsymxy ......................242

gszmxy ......................242

gT2m .......................209

gTmax .................. 192,209

gTrms .......................192

gTxgsrms ....................192

gTxgsx2mxy ..................242

gTxgsx2mz ...................231

gTxgsxmxy ...................242

gTxgsxmz ....................231

gTxgsy2mxy ..................242

gTxgsy2mz ...................231

gTxgsymxy ...................242

gTxgsymz ....................231

gTxgsz2mxy ..................242

gTxgsz2mz ...................231

gTxgszmxy ...................242

gTxgszmz ....................231

gTxmxy .....................242

gTymxy ......................242

gTzmxy ......................242

guxgTm .....................209

guygTm .....................209

guzgTm .....................209

gzlnrhomz ...................231

h22rms . . . . . . . . . . . . . . 200, 207, 208

h23rms . . . . . . . . . . . . . . 200, 207, 208

h33rms . . . . . . . . . . . . . . 200, 207, 208

hat ..................... 246,247

hcond0 .................. 184,185

hcond1 ......................184

hcond2 ......................184

hds ..................... 250,252

headt .......................110

headtt .......................110

heatmz ......................231

height eta ....................186

height ff .....................187

hhT2m . . . . . . . . . . . . . . 200, 201, 208

hhThhXm ....................200

hhTp2 . . . . . . . . . . . . . . 200, 201, 208

hhTpt . . . . . . . . . . . . . . . 200, 201, 208

hhTXm . . . . . . . . . . . . . . 200, 201, 208

hhX2m . . . . . . . . . . . . . . 200, 201, 208

hhXp2 . . . . . . . . . . . . . . 200, 201, 208

hhXpt . . . . . . . . . . . . . . . 200, 201, 208

hijij2m ......................201

hjparallelm .............. 196,206

hjperpm ................. 196,206

hjrms ................... 194,204

Hmax .......................191

hrms . . . . . . . . . . . . . . . . 200, 201, 208

hs ...................... 250,252

hse ..................... 250,252

hydro.f90 ....................173

ialive ................. 25,26,183

idiag jbm ....................100

idiff ........................143

IDL PATH ..................5,55

idx tavg ............... 30,31,183

iforce .......................186

iforce2 ......................186

iheatcond ................ 184,186

imax .........................54

in ...................... 251,252

in0 ..................... 251,253

ind ..................... 251,253

inf ..................... 251,252

init ads mol frac ..............181

init surf mol frac ..............181

initaa .......................179

initaa2 ......................180

initlncc ......................180

VARIABLE INDEX 273

initlncc2 .....................180

initlnrho .....................177

initpower ....................130

initpower2 ...................130

initss .......................178

inituu .......................176

ioc ..................... 246,247

ip ................... 35,174,181

Iring1,Iring2 .................180

isav .........................25

isave ........................182

ism .........................250

isothtop ................. 179,185

Isurf ........................227

it . . . . . . . . . . . . . . . . . . 8, 33, 34, 188

it1 ................... 25,29,182

it1d ..................... 29,182

itorder ................ 36,38,182

iuut ........................102

ivar ........................110

ivisc ........................187

iwig ........................182

ix ....................... 26,182

iy ....................... 26,182

iz ....................... 26,182

iz2 ...................... 26,182

j11rms .................. 213,216

j2 ..........................227

j2m . . . . . . . . . . . . . . . . . 192, 198, 202

j2mz .................... 233,235

jb ...................... 100,227

jb0m ................ 213,216,220

jb int ................... 192,202

jbm . . . . . . . . . . . . . . . . . 100, 192, 202

jbmh .................... 192,202

jbmn .................... 192,202

jbmphi .................. 228,229

jbms .................... 192,202

jbmxy ................... 243,244

jbmz .................... 232,234

jbrms ................... 192,202

jbtm .................... 192,202

jdel2am .....................196

jet ...................... 246,247

jj ..........................227

jm .........................198

jm2 ..................... 192,202

jmax ................ 194,198,204

jmbmz .................. 195,205

jmin ........................198

jmx ..................... 195,204

jmy ..................... 195,204

jmz ..................... 195,204

jparallelm ............... 196,206

jperpm .................. 196,206

jrms ................ 194,198,204

jx2m ........................198

jxaprms .....................197

jxarms ......................197

jxbm .................... 195,205

jxbmx ................... 195,205

jxbmy ................... 196,205

jxbmz ................... 196,205

jxbr2m .................. 196,205

jxbrmax ................. 196,205

jxbxm ................... 193,202

jxbym ................... 193,202

jxbzm ................... 193,203

jxgLamrms ...................197

jxm ..................... 198,199

jxmax ............... 194,198,204

jxmxy .......................243

jxmxz .......................240

jxmz .................... 232,234

jxp2 .................... 193,203

jxpt ..................... 193,203

jy2m ........................198

jybxm ................... 193,202

jybym ................... 193,202

jybzm ................... 193,203

jym .........................198

jymax ............... 194,198,204

jymxy .......................243

jymxz ................... 240,241

jymz .................... 232,234

jyp2 .................... 193,203

jypt ..................... 193,203

jz2m ........................198

jzbxm ................... 193,202

jzbym ................... 193,203

jzbzm ................... 193,203

jzm .........................198

jzmax ............... 194,198,204

jzmxy .......................243

jzmxz ................... 240,241

jzmz .................... 232,234

jzp2 .................... 193,203

jzpt ..................... 193,203

kforc .......................184

kap11 ............... 222,223,225

274 THE PENCIL CODE

kap11z . . . . . . . . . . . . . . 222, 224, 225

kap12 . . . . . . . . . . . . . . . 222, 224, 225

kap12z . . . . . . . . . . . . . . 222, 224, 225

kap13 . . . . . . . . . . . . . . . 222, 224, 225

kap13z . . . . . . . . . . . . . . 222, 224, 225

kap21 . . . . . . . . . . . . . . . 222, 223, 225

kap21z . . . . . . . . . . . . . . 222, 224, 225

kap22 . . . . . . . . . . . . . . . 222, 224, 225

kap22z . . . . . . . . . . . . . . 222, 224, 225

kap23 . . . . . . . . . . . . . . . 222, 224, 225

kap23z .................. 223–225

kap31 . . . . . . . . . . . . . . . 222, 223, 225

kap31z . . . . . . . . . . . . . . 222, 224, 225

kap32 . . . . . . . . . . . . . . . 222, 224, 225

kap32z . . . . . . . . . . . . . . 222, 224, 225

kap33 . . . . . . . . . . . . . . . 222, 224, 225

kap33z .................. 223–225

kapcPARA ...................223

kapcPARAz ...................223

kapcPERP1 ..................223

kapcPERP2 ..................223

kapcPERPz ..................223

kapPARA ................ 210,211

kapPARAz ............... 210,211

kapPERP ................ 210,211

kapPERP2 ...................211

kapPERPz ............... 210,211

kfountain ....................187

khor ss ......................179

kinﬂow ......................186

KK2m .......................199

KKm ........................199

Kkramersm ..................192

Kkramersmx ..................238

Kkramersmz ..................231

kmz .................... 195,205

kpeak .......................130

kx ..........................186

kx aa . . . . . . . . . . . . . . . 180, 195, 205

kx lncc ......................180

ky ..........................186

ky aa .......................180

ky lncc ......................180

kz ..........................186

kz aa .......................180

kz lncc ......................180

l1 ..........................110

l2 ..........................110

Lambzm .....................197

Lambzmz ....................197

Lamm ......................197

Lamp2 ......................197

Lampt ......................197

Lamrms .....................197

LANG ........................84

lb nxgrid .....................54

lbubble ......................188

lcalc heatcond constchi ..........184

ldamp fade ...................183

ldensity var ...................90

ldragforce dust par .............187

ldragforce gas par .............187

ldraglaw steadystate ...........187

lequidist ......................23

lﬁrst ........................110

lﬁrstpoint ....................110

lhcond global .................186

lignore Bext in b2 ..............186

lncc ........................228

lnowrite .....................174

lnrho .......................227

lnrhomax ....................191

lnrhomin ....................191

lnrhomphi ............... 228,229

lnTT ........................227

lnVpm ......................206

lout .........................110

lperi ........................174

lpress equil ...................180

lprocz slowest .............. 50,174

lpscalar sink .................187

lread oldsnap .................175

lread oldsnap nomag ...........175

lread oldsnap nopscalar .........175

lroot ........................110

lshift origin ..................175

lspecies transfer [T] ............188

lstalk ap .....................181

lstalk bb .....................181

lstalk grho ...................181

lstalk guu ....................181

lstalk relvel ..................181

lstalk rho ....................181

lstalk uu .....................181

lstalk vv .....................181

lstalk xx .....................181

lthiele [T] ....................188

luminosity ...................185

lupw lnrho ...................184

lupw ss ......................185

VARIABLE INDEX 275

luse Bext in b2 ................186

lwrite 2d ....................174

lwrite aux . . . . . . . . . . 67, 102, 174, 183

lwrite ic .....................174

lwrite phiaverages ..............29

lwrite yaverages ................29

lwrite zaverages ................29

Lxyz . . . . . . . . . . . . . . . . 23, 25, 35, 174

m..........................110

m1 .........................110

M11 ................ 212,216,219

M11cc . . . . . . . . . . . . . . . 212, 216, 219

M11ss . . . . . . . . . . . . . . . 212, 216, 219

M11z ............... 214,217,221

M12cs . . . . . . . . . . . . . . . 212, 216, 220

m2 .........................110

M22 ................ 212,216,219

M22cc . . . . . . . . . . . . . . . 212, 216, 219

M22ss . . . . . . . . . . . . . . . 212, 216, 219

M22z ............... 214,217,221

M33 ................ 212,216,219

M33z ............... 214,217,221

mach .......................227

mag ﬂux .....................209

magfricmax ..................205

MAGNETIC INIT PARS ........175

Mamax ......................190

Marms ......................190

mass ................ 191,197,199

maux .................... 32,102

maxadvec ................ 143,188

meshRemax ..................226

mgam33 ................. 223–225

mkap33 ................. 223–225

MMxm ......................199

MMym ......................199

MMzm ......................199

mpm ........................207

mpmax ......................207

mpmin ......................207

mpoly0 .................. 178,179

mpoly1 .................. 178,179

mpoly2 ......................179

mu ..................... 210,211

mu2 ........................211

mu5b2m .....................199

mu5bjm .....................198

mu5bjrms ....................198

mu5bxm .....................199

mu5m .......................198

mu5rms .....................198

muc1 .......................223

muc2 .......................223

mucz .......................223

mumz .......................235

muSm ......................198

muSrms .....................198

muz .................... 210,211

mvar ................. 32,79,175

mx .................. 26,110,111

my .................. 26,110,111

mz .................. 26,110,111

n..........................110

n1 ..........................110

n1s ................. 245,248,250

n2 ..........................110

nfr ..................... 246–249

ngam33 ................. 223–225

nil . . . . . . . . . . . . . . 246, 247, 251, 253

nil’,’ .................... 248,249

nkap33 .................. 223–225

noentropy.f90 .................173

nogpu.f90 ....................173

nohydro.f90 ..................173

nopower spectrum.f90 ...........173

noyinyang.f90 .................173

noyinyang mpi.f90 .............173

npm ........................207

nprocy ................... 50,174

nprocz .......................50

nr1 .........................246

nr directions ...................54

nt ..................... 8,36,181

nu ..................... 187,221

nu epicycle ............... 178,187

nu hyper2 ....................187

nu hyper3 ....................187

nu LES .....................226

nu tdep ......................226

num ........................226

numx .......................239

nuQ ........................221

nusmagm ....................226

nusmagmax ..................226

nusmagmin ..................226

nv ..........................110

nvar ...................... 26,84

nx . . . . . . . . . . . . . 28, 29, 103, 110, 111

nxgrid ................ 53,54,110

ny .................28,29,110,146

276 THE PENCIL CODE

nygrid .......................41

nz . . . . . . . . . . . . . . . . . 28, 29, 110, 146

nzgrid ........................41

o2 ..........................227

o2m ........................190

o2mz .......................229

odel2um .....................190

ogux2mz .....................230

oguxmz ......................230

oguy2mz .....................230

oguymz ......................230

oguz2mz .....................230

oguzmz ......................230

omax .......................190

Omega ......................183

omega ff .....................187

omumz ......................189

oo ..........................227

orms ........................190

ou0 ..................... 251,253

ou int .......................190

oud ..................... 251,253

ouf ..................... 251,252

oum ..................... 25,190

oumphi ......................190

oumx .......................237

oumxy .......................241

oumxz .......................239

oumy .......................236

oumz .......................230

out . . . . . . . . . . 245, 247–249, 251, 252

out1 ........................182

out2 ........................182

outm ........................188

ovr . . . . . . . . . . . . . . 245, 247, 251, 252

ox2m .......................190

ox2mx .......................237

ox2mz .......................230

oxdivu2mz ...................231

oxdivumz ....................230

oxmxy .......................241

oxmz ........................230

oxoym .......................190

oxozm .......................190

oxuxxmz .....................230

oxuyxmz .....................230

oxuzxm ......................190

oxuzxmz .....................230

oy2m .......................190

oy2mx .......................237

oy2mz .......................230

oydivu2mz ...................231

oydivumz ....................230

oymxy .......................241

oymz ........................230

oyozm .......................190

oyuxymz .....................230

oyuyymz .....................230

oyuzym ......................190

oyuzymz .....................230

oz2m .......................190

oz2mx .......................237

oz2mz .......................230

ozdivu2mz ...................231

ozdivumz ....................230

ozmxy .......................241

ozmz ........................230

p. . . . . . . . . . . . . . . . 244, 246–249, 251

p1D .................... 250,252

particles adsorbed.f90 ..........173

particles chemistry.f90 ..........173

particles surfspec.f90 ...........173

PATH.................... 5,6,12

pdivum . . . . . . . . . . . . . . 191, 199, 206

peffmxz ......................241

PENCIL HOME . . . . . . . . . . . . 5, 6, 76

PENCIL HOST ID ..............18

pertss .......................178

pfc ..................... 246–249

pfe ..................... 250,252

phi11 ................... 212,215

phi12 ................... 212,215

phi21 ................... 212,215

phi22 ................... 212,215

phi32 ................... 212,215

phibmx .................. 196,205

phibmy .................. 196,205

phibmz .................. 196,205

phibzm ......................201

phibzmz .....................202

phiK .................... 212,215

phiM ................... 212,215

phim .......................201

phiMK .................. 212,215

phimphi .....................228

phip2 .......................201

phipt .......................201

placeholder ...................188

polytrm ......................207

pot ..................... 250,252

VARIABLE INDEX 277

power spectrum.f90 ............173

Poynting .....................227

poynxmxy ................ 243,244

poynymxy ................ 243,244

poynzmxy ................ 243,244

poynzmz ................. 233,235

pp . . . . . . . . . . . . . . . . . . 227, 247, 248

ppm . . . . . . . . . . . . . 191, 199, 210, 226

ppmx ................... 237,239

ppmy ................... 236,237

ppmz ................... 231,235

pr1mz .......................235

pretend lnTT .................176

pscalar diff ..................186

PSCALAR INIT PARS ..........175

pscalar sink rate ..............187

psi11 ................... 212,215

psi12 ................... 212,215

psi21 ................... 212,215

psi22 ................... 212,215

puzmz .......................235

pvzm .......................190

pvzmxy ......................241

pwd .................... 250,252

q2m ........................190

qam ........................206

qem ........................206

qfm .........................190

qfviscm ......................226

qmax . . . . . . . . . . . . . 54, 190, 196, 201

qom ........................190

qpm ........................206

qpmz .......................235

Qrad .......................227

qrms ................ 190,196,201

qsatmin .....................201

qsatrms .....................201

qshear .................. 181,187

qsm ........................206

quxom ......................190

qxmax ......................201

qxmin .......................201

qymax ......................201

qymin .......................201

qzmax .......................201

qzmin .......................201

rext ........................186

rff .........................187

rint ........................186

radius ......................180

radius ss ....................178

random gen .............. 175,183

rcool ........................185

rcylmphi .....................228

rdamp ......................183

rdampext ....................183

rdampint ....................183

rdivum ......................189

REAL PRECISION ......... 52,146

reinitialize lncc ................186

relhel ................... 151,187

relhel uu .....................130

Remz .......................230

Reshock .....................226

rho .........................227

rho0 ................ 177,184,187

rho2mx ......................231

rho2mz ......................231

rho left ......................177

rho right .....................177

rhoccm ......................196

rhom ...............8,25,191,197

rhomax .................. 191,199

rhomin .................. 191,199

rhomphi ................. 228,229

rhomx .......................237

rhomxmask ..................191

rhomxy ......................242

rhomxz ......................239

rhomy .......................236

rhomz .......................231

rhomzmask ...................191

rlx2m .......................190

rlxm ........................190

rly2m .......................190

rlym ........................190

rlz2m .......................190

rlzm ........................190

Rmesh ......................188

Rmesh3 .....................188

Rmmz .......................195

rmphi .......................228

Rring1,Rring2 ................180

rumax ......................189

rux2m .......................189

rux2mx ......................237

rux2mxy .....................242

rux2mz ......................230

ruxm .......................189

278 THE PENCIL CODE

ruxmx .......................237

ruxmxy ......................242

ruxmz .......................230

ruxtot .......................189

ruxuy2mz ....................230

ruxuym ......................190

ruxuymx .....................237

ruxuymxy ....................242

ruxuymz .....................230

ruxuz2mz ....................230

ruxuzm ......................190

ruxuzmx .....................237

ruxuzmxy ....................242

ruxuzmz .....................230

ruy2m .......................189

ruy2mx ......................237

ruy2mxy .....................242

ruy2mz ......................230

ruym .......................189

ruymx .......................237

ruymxy ......................242

ruymz .......................230

ruyuz2mz ....................230

ruyuzm ......................190

ruyuzmx .....................237

ruyuzmxy ....................242

ruyuzmz .....................230

ruz2m .......................189

ruz2mx ......................237

ruz2mxy .....................242

ruz2mz ......................230

ruzdownmz ...................229

ruzm .......................189

ruzmx .......................237

ruzmxy ......................242

ruzmz .......................230

ruzupmz .....................229

s. . . . . . . . . . . . . . . . 244, 246–249, 251

s+f ..................... 248,249

s0d . . . . . . . . . . 244, 246, 247, 249, 251

s2kzDFm . . . . . . . . . . . . 212, 216, 219

sa2 ..................... 246,247

sds ..................... 247–249

sep ..................... 248,249

set . . . . . . . . . . 245, 247–249, 251, 252

sf . . . . . . . . . . . . . . . 244, 247, 249, 251

sfr ..................... 246–249

Shchm ......................206

shock .......................227

shockmax ....................209

shx .........................245

shy .........................245

shz .........................245

Sij2m .......................226

slice position . . . . . . . . . . . 26, 27, 182

slo ..................... 245,247

slope c max ..................226

slp .........................245

spd ..................... 246,247

spr ..................... 245,246

spt ..................... 248,249

sr1 .........................246

ss . . . . . . . . . . . . . . . 227, 244, 246–248

ss2m .................... 191,199

ss2mx .......................237

ss2mz .......................231

sse ..................... 248,249

ssm . . . . . . . . . . . . . . . . 8, 191, 199, 210

ssmax .......................192

ssmin .......................192

ssmphi .................. 228,229

ssmx ........................237

ssmxy ................... 200,242

ssmxz ................... 200,240

ssmy ........................236

ssmz .................... 231,235

ssruzm ......................191

ssuzm .......................191

sT . . . . . . . . . . . 245, 246, 248–250, 252

StokesImxy ............... 243,244

StokesQ1mxy ............. 243,244

StokesQmxy .............. 243,244

StokesU1mxy ............. 243,244

StokesUmxy .............. 243,244

strTpt .......................200

strXpt .......................200

StS ..................... 251,252

t...................8,25,110,188

tauheat buffer .................185

tauhmin .....................191

tauqmax .....................201

tavg .................. 30,31,183

tdamp .......................183

Tdxpm ......................209

Tdypm ......................209

Tdzpm ......................209

tensor pscalar diff .............186

test chemistry.f90 ..............173

thcool .......................210

theta ........................183

VARIABLE INDEX 279

timestep.f90 ..................173

timestep strang.f90 .............173

timestep subcycle.f90 ...........173

tmax ........................182

tot ang mom ..................190

total carbon sites ..............181

totmass ......................191

Trms .......................209

TrSigmapm ..................206

ts ...........................44

TT .........................227

TT2m .......................209

TT2mx ......................237

TT2mz .................. 231,235

TTheat buffer .................185

TTm . . . . . . . . . . . . . 192, 209, 210, 226

TTmax . . . . . . . . . . . 192, 209, 210, 226

TTmin . . . . . . . . . . . 192, 209, 210, 226

TTmx ................... 237,239

TTmxy .................. 242,244

TTmxz .................. 240,241

TTmy ................... 236,237

TTmz ................... 231,235

ttransient ....................183

TTtop ................... 191,200

TTzmask ....................209

TugTm ......................209

Tugux uxugTm ................209

Tuguy uyugTm ................209

Tuguz uzugTm ................209

u0rms ................... 213,216

u11rms .................. 213,216

u12rms .................. 213,216

u1u23m .....................189

u1u32m .....................189

u2 ..........................227

u21rms .................. 213,216

u22rms .................. 213,216

u2m ........................188

u2mphi ......................228

u2mz .......................229

u2tm .......................188

u2u13m .....................189

u2u31m .....................189

u3u12m .....................189

u3u21m .....................189

uabxmz .................. 232,233

uabymz .................. 232,233

uabzmz .................. 232,233

uam .................... 193,203

uamz ................... 232,234

ubbzm .................. 192,202

ubm .................... 193,202

ubmz ................... 232,234

ubs ..................... 251,253

udpxxm .....................191

ufpresm .....................192

ufviscm ......................226

uglnrhom ....................191

uglnrhomz ...................231

ugm ........................201

ugrhom .................. 191,197

ugrhomz .....................231

ugu2m ......................190

ugurmsx .....................190

uguxmxy .....................241

uguymxy .....................241

uguzmxy .....................242

ujm .................... 193,203

ujxbm ................... 196,205

umamz ......................189

umax ..................... 8,188

umbmz ......................189

umin .......................188

umx ..................... 29,189

umxbmz .....................189

umy ..................... 29,189

umz ..................... 29,189

unit density ............... 37,175

unit length ................ 37,175

unit system ................ 37,175

unit temperature . . . . . . . . 36, 37, 175

unit velocity ............... 37,175

uotm ........................188

upmphi ......................228

urand .......................176

urmphi ......................228

urms . . . . . . . . . . . . . . . . 8, 25, 130, 188

urmsx .......................188

urmsz .......................188

ursphmphi ...................228

uthmphi .....................228

uu .........................227

uu left ......................176

uu right .....................176

uumphi .....................228

uusphmphi ...................228

uut .........................102

ux0m ................... 213,216

ux0mz ......................221

280 THE PENCIL CODE

ux11m .................. 213,216

ux2ccm ......................189

ux2m .......................189

ux2mx ......................237

ux2mxy ......................242

ux2mxz ......................239

ux2mz ......................230

ux2ssm ......................189

uxbm ................... 195,205

uxbmx .................. 195,205

uxbmy .................. 195,205

uxbmz .................. 195,205

uxbxm .................. 193,202

uxbxmz .................. 232,234

uxbym .................. 193,202

uxbymz .................. 232,234

uxbzm .................. 193,202

uxbzmz .................. 232,234

uxglnrym ....................190

uxm ........................189

uxmax ......................189

uxmin .......................189

uxmx .......................237

uxmxy .......................241

uxmxz .......................239

uxmy .......................236

uxmz .......................229

uxp2 ........................188

uxpt ........................188

uxrms .......................188

uxTm .......................209

uxTmz ......................235

uxTTmx .....................238

uxTTmxy ....................242

uxTTmz .....................231

uxuycsm .....................189

uxuydivum ...................190

uxuym ......................189

uxuymx .....................237

uxuymxy .....................241

uxuymxz .....................239

uxuymz ......................230

uxuzm ......................189

uxuzmx ......................237

uxuzmxy .....................241

uxuzmxz .....................239

uxuzmz ......................230

uxxrms ......................191

uxzrms ......................191

uy0m ................... 213,216

uy0mz ......................221

uy11m .................. 213,216

uy2ccm ......................189

uy2m .......................189

uy2mx ......................237

uy2mxy ......................242

uy2mxz ......................239

uy2mz ......................230

uy2ssm ......................189

uybxm .................. 193,202

uybxmxz ................. 240,241

uybxmz .................. 232,234

uybym .................. 193,202

uybymz .................. 232,234

uybzm .................. 193,202

uybzmxz ................. 240,241

uybzmz .................. 232,234

uyglnrxm ....................190

uygzlnrhomz ..................231

uym ........................189

uymax ......................189

uymin .......................189

uymx .......................237

uymxy .......................241

uymxz .......................239

uymy .......................236

uymz .......................229

uyp2 ........................188

uypt ........................188

uyrms .......................188

uyTm .......................209

uyTmz ......................235

uyTTmx .....................238

uyTTmxy ....................242

uyTTmz .....................231

uyuzm ......................189

uyuzmx ......................237

uyuzmxy .....................241

uyuzmxz .....................239

uyuzmz ......................230

uyxuzxmz ....................230

uyyrms ......................191

uyyuzymz ....................230

uyzrms ......................191

uyzuzzmz ....................230

uz0mz .......................221

uz2m .......................189

uz2mx ......................237

uz2mxy ......................242

uz2mxz ......................239

VARIABLE INDEX 281

uz2mz .......................230

uzbxm .................. 193,202

uzbxmz .................. 232,234

uzbym .................. 193,202

uzbymz .................. 232,234

uzbzm ................... 193,202

uzbzmz .................. 232,234

uzdivum .....................190

uzdivumz ....................230

uzdownmz ...................229

uzgylnrhomz ..................231

uzjx1z .......................220

uzjx2z .......................220

uzjx3z .......................221

uzjx4z .......................221

uzjy1z .......................220

uzjy2z .......................220

uzjy3z .......................221

uzjy4z .......................221

uzjz1z .......................220

uzjz2z .......................221

uzjz3z .......................221

uzjz4z .......................221

uzm ........................189

uzmax ......................189

uzmin .......................189

uzmphi ......................228

uzmx .......................237

uzmxy .......................241

uzmxz .......................239

uzmy .......................236

uzmz .......................229

uzp2 ........................188

uzpt ........................188

uzrms .......................189

uzTm .......................209

uzTmz ......................235

uzTTmx .....................238

uzTTmxy ....................242

uzTTmz .....................231

uzupmz .....................229

uzyrms ......................191

v. . . . . . . . . . . . . . . . 245, 246, 248–251

v3 ...................... 248–251

vAm ........................198

vAmax .............. 194,198,204

vAmin ......................198

vAmxz .................. 240,241

vArms ................... 194,204

visc heatm ...................226

vmagfricmax .................195

vmagfricmz ..................233

vmagfricrms ..................195

vol .........................191

vpx2m ......................207

vpxm .......................207

vpxmax ......................207

vpxmin ......................207

vrelpabsm ....................207

wforc .......................184

walltime .....................188

wcool .......................185

wdamp .................. 183,184

wheat .......................185

width ff .....................187

widthaa .....................180

widthlnrho ...................177

widthss . . . . . . . . . . . . . . 178, 184, 185

widthuu .....................176

win ..................... 251,253

wr1,wr2 .....................180

write slices ....................27

wsnaps.f90 ...................182

xi ..........................221

xiQ .........................221

xp2m .......................207

xpm .................... 206,207

xpmax ......................206

xpmin .......................206

xy ..........................182

xy2 .........................182

xyz0 .................. 23,25,174

xyz star ......................25

yH .........................227

yHm .................... 192,210

yHmax .................. 192,209

yHmin ......................210

yinyang.f90 ...................173

yinyang mpi.f90 ...............173

yy ...................... 247,249

z0aa ........................180

z1 ..........................177

z2 ..........................178

zbot slice .............. 26,28,182

zeta .................... 187,221

zetaQ .......................221

zheat buffer ..................185

zmphi .......................228

282 THE PENCIL CODE

zref .................... 177,187

ztop slice .............. 26,28,182

Index

This index contains options, names, deﬁnitions and commands. Files and variables have

their own indexes.

’VAR10’ ......................45

.r ...........................45

.run .........................45

.svn .........................12

/trimall ......................45

2N-scheme ...................159

6th-order derivatives . . . . . . . . . . . 156

pc mkproctree 16 ..............147

adapt-mkﬁle...................78

adapt-mkﬁle ................ 22,89

anelastic......................67

Auto-tests....................108

autoconf......................89

Autoconf......................89

Autoconf/automake . . . . . . . . . . . . . . 89

Averages .................. 29,30

Azimuthal averages . . . . . . . . . . . . . 29

bandwidth ....................50

Bash.......................5,76

bash .........................44

bc ...........................44

Beowulf clusters . . . . . . . . . . . . . . . . 50

Bidiagonal scheme . . . . . . . . . . . . . 158

bin/pc run ....................83

Boundary conditions . . . . . . . . . . . . . 39

Bourneshell....................5

C . . . . . . . . . . . . . . . . . . . . . viii, 1, 111

Cdata.......................110

cgs units . . . . . . . . . . . . . . . . . . 36, 175

Changes.....................128

Check-in details . . . . . . . . . . . . . . . . 93

ChiralMHD...................69

Coding standards . . . . . . . . . . . 99, 124

Combustion ...................66

Comments ...................125

Coordinate systems . . . . . . . . . . . . . 59

copy-proc-to-proc ................31

Coriolis force . . . . . . . . . . . . . . . . . 183

Cosmicrays ...................69

Courant number . . . . . . . . . . . . . . . . 36

Covariant derivatives . . . . . . . . . . . 165

Cron........................108

crontab -e ....................108

CSH........................ viii

Csh................... 1,5,12,76

csh ..........................76

Curvilinear coordinates . . . . . . 59, 165

CVS ..........................2

CVS .........................vii

Cvs..........................11

cvs-add-rundir .................32

Daainit......................148

Data directory . . . . . . . . . . . . . . . . . 14

Data explorer . . . . . . . . . . . . . . . . 1, 41

dataﬁles......................25

Density initpars ..............176

Density runpars ..............184

double precision . . . . . . . . . . . . 51, 146

Download . . . . . . . . . . . . . . . . 2, 44, 76

Download forbidden . . . . . . . . . . . . . 76

DX . . . . . . . . . . viii, 1, 5, 12, 32, 41, 42

Emacs settings . . . . . . . . . . . . . . . . 127

Entropy ......................61

Entropy . . . . . . . . . . . . . . . . 15, 40, 61

Entropy.f90....................27

Entropy initpars..............178

Entropy runpars..............184

Equation of state . . . . . . . . . . . . . . . 63

Error, diffusive . . . . . . . . . . . . . . . . 160

Etatest......................148

f-array ......................102

f90 ....................... 21,22

F95....................... viii,1

f95 ..........................21

FAQ .........................76

FBCX1......................148

FBCX2 2 ....................148

ff ...........................45

ff.varname ....................46

FFT .........................13

Fftpack.......................52

Filters ......................139

Flag .................... 174,181

283

284 THE PENCIL CODE

Fluxrings....................130

Forcing run pars . . . . 36, 150, 151, 186

Fortran record . . . . . . . . . . . . . . 26, 30

Fortran record . . . . . . . . . . . . . . . . . 26

fp-array .....................103

Frequently Asked Questions . . . . . . . 76

ftp ..........................44

Fully qualiﬁed host name . . . . . . . . . 18

G77 .........................78

G95 ...................... 52,77

GDL.........................42

Gfortran . . . . . . . . . . . . . . . . . . viii, 52

Ghostpoints...................39

Ghost zones . . . . . . . . . . . . . . . . 39, 50

Git ...........................2

Git .........................2,3

git ...........................3

Glibc ........................77

Gnu Data Language . . . . . . . . . . . . . 42

GNUgcc..................... viii

Gnuplot ................... 15,41

gnuplot .......................44

Grav initpars ................177

Grav r .......................13

Grav run pars . . . . . . . . . . . . 148, 187

Gravitational Waves . . . . . . . . . . . . . 73

Gravity.......................13

Gravity simple.................13

grep . . . . . . . . . . . . . . . . . . . viii, 97, 98

grid, nonuniform . . . . . . . . . . . . . . . 23

h-index.......................93

Hydro.f90.....................27

Hydro initpars ...............176

Hydro runpars ...............183

hyperdiffusivity . . . . . . . . . . . . . . . 139

Hyperviscosity . 139, 141–143, 156, 158

Icc ..........................77

IDL viii, 1, 5, 8, 9, 12, 15, 27, 28, 30, 32,

42–44, 53, 55

IDL ........................151

idl ..........................44

Ifc...........................77

Ifort ...................... 77,78

ifort .........................52

incompressible . . . . . . . . . . . . . . . . . 67

Init pars . . . . . . . . . . . . . . . 34, 35, 174

Initial conditions . . . . . . . . . . . . . . 129

InitialCondition module . . . . . . . . . 106

Interlocked ﬂux rings . . . . . . . . . . . 130

Interstellar . . . . . . . . . . . . . . . . . . . . 15

IO...................... 110,111

Io mpiodist.f90 . . . . . . . . . . . . . . . . . 16

Ionization . . . . . . . . . . . . . . . . . 64, 161

Ionization.f90 . . . . . . . . . . . . . . . 36, 37

Janus..................... 21,22

ldensity ......................90

Linux...................... 1,77

locate mpif.h ...................82

Magnetic ....................100

Magnetic helicity . . . . . . . . . . . . . . . vii

Magnetic.f90 . . . . . . . . . . . . . . . 27, 28

Magnetic init pars . . . . . . . . . . . . . 179

Magnetic run pars . . . . . . . . . 148, 186

Make . . . . . . . . . . . . . . . . 1, 13, 22, 79

make ................ 6,13,19,20

make clean ....................77

Makeﬁle . . . . . . . . . . . . . . 6, 14, 21, 81

Makeﬁle ......................20

Manual . . . . . . . . . . . . . . . . . iv, 91, 106

mesh, nonuniform . . . . . . . . . . . . . . 23

Message passing interface . . . . . . . . 49

Module...................... viii

Module.h .....................77

Modules ......................13

Modules . . . . . . . . . . . . . . . . . . viii, 13

MPEG .......................27

Mpeg encode ..................27

MPI . . . . vii, 1, 9, 13–15, 21, 49, 78, 89

mpif90 -show ..................82

mpif90 -showme ................82

mpirun .......................14

Namelist .....................32

Namelists.....................34

Networks .....................41

NEWDIRﬁle ..................34

Newphysics ..................106

Noentropy . . . . . . . . . . . . . . 15, 40, 61

NOERASEﬁle .................87

Nogravity.....................13

Noionization.f90 . . . . . . . . . . . . . 36, 37

Nomodule.f90 . . . . . . . . . . . . . . . . . . 77

Nonewphysics . . . . . . . . . . . . . . . . 106

nonuniform grid . . . . . . . . . . . . . . . . 23

Nospecial.f90 . . . . . . . . . . . . . 105, 106

INDEX 285

octave ........................44

Onsager ......................22

OpenDX.......................1

Option ‘–host-id’ ................18

Option ‘–max-level’ .............109

Option ‘–use-pc’ ...............109

Option ‘–use-pc auto-test’ .........21

Option ‘-b’ .....................21

Option ‘-D’ ...................109

Option ‘-f’ ....................108

Option ‘-fast’ ...................22

Option ‘-fno-second-underscore’ . . 77, 78

Option ‘-H’ ................ 18,109

Option ‘-l’ ....................108

Option ‘-lmpi’ ..................21

Option ‘-m’ ...................109

Option ‘-N’ ...................109

Option ‘-nothreads’ ..............78

Option ‘-O2 -u’ .................21

Option ‘-O3’ ................ 21,80

Option ‘-qextname’ ..............77

Option ‘-T’ ...................109

Option ‘-t’ ....................109

Option ‘-Uc’ ..................109

Option ‘-Wa,–max-level=2’ ........109

Option ‘/png’ ..................27

Option ‘a’ .....................39

Option ‘a2’ ....................40

Option ‘c1’ . . . . . . . . . . . . 40, 134, 185

Option ‘c2’ ................ 40,184

Option ‘ce’ .....................40

Option ‘cT’ ....................40

Option ‘db’ ....................40

Option ‘g’ .....................40

Option ‘hs’ ....................40

Option ‘nohydro’ ...............186

Option ‘p’ .....................39

Option ‘pot’ ...................134

Option ‘pwd’ ..................134

Option ‘s’ .....................40

Option ‘she’ ....................40

Particles . . . . . . . . . . . . . . . . . . 70, 148

Particles ads init pars . . . . . . . . . . 181

Particles ads run pars . . . . . . . . . . 188

Particles chem init pars . . . . . . . . . 181

Particles chem run pars . . . . . . . . . 188

Particles run pars . . . . . . . . . . . . . 187

Particles stalker init pars . . . . . . . 181

Particles surf init pars . . . . . . . . . . 181

Particles surf run pars . . . . . . . . . . 188

pc jobtransfer..................34

pc auto-test . . . . . . . . . . . 20, 21, 93, 108

pc auto-test –help ........... 21,108

pc build ................... 17,20

pc build –cleanall ..............109

pc build –help ..................20

pc get quantity .............. 44,45

pc jobtransfer ..................34

pc mkdatadir ...................7

pc newrun .....................7

pc read const ..................46

pc read param .................46

pc read pvar ...................46

pc read t ......................46

pc read var ................. 44–46

pc read var raw ............. 44,46

pc read xyaver .................46

pc read xzaver .................46

pc read yzaver .................46

pc run .............. 17,19,20,83

pc run –help ...................20

pc setupsrc . . . . . . . . . 12, 32, 52, 76, 77

pc svnup .......................3

pc svnup -val ...................3

pc tsnap ......................26

Pencilcase ...................103

Pencilcheck ..................104

PencilCode ...................89

Pencil consistency check . . . . . . . . . 104

Pencildesign ..................12

pencil-test . . . . . . . . . . . . . 21, 108, 109

pencil-test –help ............ 21,108

pencil check small ..............67

Pencils ................... vii,103

Perl ....................viii,1,12

perldoc Pencil::ConﬁgFinder .......17

perldoc PENCIL::ConﬁgParser .....17

Planet solution . . . . . . . . . . . . . . . . 136

PNG.........................27

Polytropic atmosphere . . . . . . . . . . 132

Potential-ﬁeld boundary condition . 134

power ..................... 53,54

pretend lnTT .............. 62,176

Programming style . . . . . . . . . . 99, 124

Pscalar......................106

Pscalar initpars ..............180

Pscalar runpars ..............186

Python ...................... viii

Python .......................46

Radiative transfer . . . . . . . . . . 66, 162

286 THE PENCIL CODE

Readline......................44

Regridding...................146

Remeshing...................146

RERUNﬁle ...................34

restart-new-dir ../32c ...........147

Restarting . . . . . . . . . . . . 40, 147, 148

rlwrap .......................44

Rundirectory...................6

run.x ........................30

Run pars . . . . 26–28, 34, 147, 181, 183

Runge-Kutta .................159

Runge-Kutta time step . . . . . . . . . . . 38

Runge-Kutta-Fehlberg time step . . . 38

Scripts .......................31

Setup . . . . . . . . . . . . . . . . . . . 5, 42, 76

Shear........................40

Shear initpars................180

Shear run pars . . . . . . . . . . . . 148, 187

Shock viscosity . . . . . . . . . . . . . . 37, 63

SIunits .................. 36,175

Sixth-order derivatives . . . . . . . . . . 156

sliceﬁles .....................28

Slice ﬁles . . . . . . . . . . . . . . . . . . 26, 27

Special module . . . . . . . . . . . . . . . . 105

start.csh ......................40

Stdout .......................25

Stratiﬁcation . . . . . . . . . . . . . . . . . 131

structure ......................55

Style . . . . . . . . . . . . . . . . . . . 3, 99, 124

Sub.........................111

summarize-history ..............34

svn . . . . . . . . . . . . . . . . . . 2–4, 14, 119

Svn 2–4, 11, 14, 31, 32, 80, 119, 174, 181

svn ...........................3

svn annotate src/*.f90 ............v

svn up sourceme.csh .............88

svn up sourceme.sh ..............88

svn update ...................109

svn update -r ##### ..............4

Svn/git ......................2,3

Syscalls ......................77

tab ..........................99

Tab characters . . . . . . . . . . . . . . . . 124

tag names .....................45

Tcsh..........................5

Testﬁeld method . . . . . . . . . . . . 73, 147

Timeaverages .................30

Time step . . . . . . . . . . . . . . . . . 38, 159

Toroidal averages . . . . . . . . . . . . . . . 29

touch NEWDIR .................34

touch NOERASE ..............175

touch RELOAD ................181

uname .......................22

Underscore problem . . . . . . . . . . . . . 78

Units .................... 36,175

Unix..........................1

Upwinding . . . . . . . . . . . . . 37, 97, 157

use .........................110

Vector potential . . . . . . . . . . . . . . . . 61

Videoﬁles.....................26

Viscosity . . . . . . . . . . . . . . . . . . . 37, 63

Viscosity run pars . . . . . . . . . 148, 187

Weylgauge....................61

Whitespace...................124

Xlf ..........................77

Xmgrace......................15

INDEX 287

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