[Commits] [svn:einsteintoolkit] www/publications/2013_MHD/ (Rev. 967)
rhaas at tapir.caltech.edu
rhaas at tapir.caltech.edu
Mon Apr 22 22:15:06 CDT 2013
User: rhaas
Date: 2013/04/22 10:15 PM
Modified:
/publications/2013_MHD/
index.php
Log:
add cost estimates to mhd page, update title and abstract
File Changes:
Directory: /publications/2013_MHD/
==================================
File [modified]: index.php
Delta lines: +51 -44
===================================================================
--- publications/2013_MHD/index.php 2013-04-23 01:35:44 UTC (rev 966)
+++ publications/2013_MHD/index.php 2013-04-23 03:15:06 UTC (rev 967)
@@ -4,38 +4,45 @@
<b><font color="red">THIS IS WORK IN PROGRESS</font></b>
<ul>
- <li>Bruno C Mundim</li>
- <li>Joshua Faber</li>
- <li>Scott Noble</li>
- <li>Tanja Bode</li>
- <li>Roland Haas</li>
- <li>Frank Löffler</li>
- <li>Philipp Mösta</li>
- <li>Christian D. Ott</li>
- <li>Christian Reisswig</li>
- <li>Erik Schnetter</li>
+<li>Philipp Mösta</li>
+<li>Bruno C. Mundim</li>
+<li>Joshua A. Faber</li>
+<li>Roland Haas</li>
+<li>Scott C. Noble</li>
+<li>Tanja Bode</li>
+<li>Frank Löffler</li>
+<li>Christian D. Ott</li>
+<li>Christian Reisswig</li>
+<li>Erik Schnetter</li>
</ul>
<p>
-We discuss the new general relativistic magnetohydrodynamics (MHD) capabilities
-of the Einstein Toolkit, a community-driven, free, publicly available code,
-developed by a collaboration of scientists from across the world, that can be
-used to perform numerical relativistic simulations. Our code is built upon
-previous Toolkit releases, and includes the ability to evolve magnetized
-fluids in the ideal magnetohydrodynamics limit in fully relativistic dynamical
-spacetimes using the same shock-capturing techniques previously applied to
-hydrodynamical evolution. In order to maintain the divergence-free character
-of the magnetic field, the code implements both hyperbolic divergence
-cleaning and constraint transport schemes. We present test results for a
-number of MHD tests in Minkowski and curved spacetimes. Minkowski tests
-include aligned and oblique shocks, cylindrical explosions, magnetic rotors,
-Alfven waves and advected loops, as well as a set of tests designed to study
-the response of the divergence cleaning scheme to numerically generated
-monopoles. Dynamical tests include spherical Bondi accretion onto a black hole
-as well as the collapse of a rotating neutron star. Our results agree with
-analytical solutions where such results are available, and we find the expected
-convergence as well. All data and files used to generate results are included
-in a public webpage, so users may perform their own testing and validation as
-an introduction to the public code. </p>
+We present the new general-relativistic magnetohydrodynamics (GRMHD)
+capabilities of the Einstein Toolkit, an open-source community-driven
+numerical relativity and computational relativistic astrophysics
+code. The GRMHD extension of the Toolkit builds upon previous releases
+and implements the evolution of relativistic magnetised fluids in the
+ideal MHD limit in fully dynamical spacetimes using the same
+shock-capturing techniques previously applied to hydrodynamical
+evolution. In order to maintain the divergence-free character of the
+magnetic field, the code implements both hyperbolic divergence
+cleaning and constrained transport schemes. We present test results
+for a number of MHD tests in Minkowski and curved spacetimes.
+Minkowski tests include aligned and oblique planar shocks, cylindrical
+explosions, magnetic rotors, Alfv\'en waves and advected loops, as
+well as a set of tests designed to study the response of the
+divergence cleaning scheme to numerically generated monopoles. We
+study the code's performance in curved spacetimes with spherical
+accretion onto a black hole on a fixed background spacetime and in
+fully dynamical spacetimes by evolutions of a magnetised polytropic
+neutron star and of the collapse of a magnetised stellar core. Our
+results agree well with exact solutions where these are
+available and we demonstrate convergence. All code and input files
+used to generate the results are available on
+<a href="http://einsteintoolkit.org">http://einsteintoolkit.org</a>.
+This makes our work fully
+reproducible and provides new users with an introduction to
+applications of the code.
+</p>
<ul>
<li>doi: <a href=""></a></li>
@@ -55,8 +62,8 @@
<a href="par/monopole/monopole-gauss.par">monopole-gauss.par</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>16 cores, 200 min</td></tr>
+ <tr><th>memory </th><td>500 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Planar MHD Shocktubes</h4>
@@ -75,8 +82,8 @@
<a href="par/shocktubes/balsara5_2d.par">balsara5_2d.par</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>1D: 2 cores, 2D: 16 cores, 240 min</td></tr>
+ <tr><th>memory </th><td>1D: 120 MB per core, 2D: 520 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Cylindrical Shocks</h4>
@@ -85,8 +92,8 @@
<a href="par/cylexp/cylexp_tvd_mc2_hlle.rpar">cylexp_tvd_mc2_hlle.rpar</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>4 cores, 160 min</td></tr>
+ <tr><th>memory </th><td>600 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Magnetic Rotor</h4>
@@ -95,8 +102,8 @@
<a href="par/rotor/rotor.rpar">rotor.rpar</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>4 cores, 290 min</td></tr>
+ <tr><th>memory </th><td>800 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Alfvén Wave</h4>
@@ -112,8 +119,8 @@
<a href="par/alfvenwave/alfvenwave2d_80_60.par">alfvenwave2d_80_60.par</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>1D: 4 cores, 60min, 2D: 4 cores, 220 min</td></tr>
+ <tr><th>memory </th><td>1D: 12 MB per core, 2D: 60MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Loop advection</h4>
@@ -127,16 +134,16 @@
<a href="par/advloop/advectedloop3D_vz.par">par/advloop/advectedloop3D_vz.par</a>
</td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>36 cores, 250 min</td></tr>
+ <tr><th>memory </th><td>100 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Bondi Inflow</h4>
<table>
<tr><th>parfile generator </th><td><a href="par/bondi/BondiFlowBase.rpar">BondiFlowBase.rpar</a></td></tr>
<tr><th>thornlist</th><td><a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2013_05/einsteintoolkit.th">Einstein Toolkit 2013_05 release</a></td></tr>
- <tr><th>CPU time </th><td>x SU</td></tr>
- <tr><th>memory </th><td>x GB</td></tr>
+ <tr><th>CPU time </th><td>48 cores, 420 min</td></tr>
+ <tr><th>memory </th><td>350 MB per core</td></tr>
<tr><th>Notes </th><td>...</td></tr>
</table>
<h4>Magnetized TOV</h4>
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