The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project. (arXiv:1904.04923v1 [astro-ph.HE])

The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project. (arXiv:1904.04923v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Porth_O/0/1/0/all/0/1">Oliver Porth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_K/0/1/0/all/0/1">Koushik Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayan_R/0/1/0/all/0/1">Ramesh Narayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gammie_C/0/1/0/all/0/1">Charles F. Gammie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mizuno_Y/0/1/0/all/0/1">Yosuke Mizuno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anninos_P/0/1/0/all/0/1">Peter Anninos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baker_J/0/1/0/all/0/1">John G. Baker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bugli_M/0/1/0/all/0/1">Matteo Bugli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chan_C/0/1/0/all/0/1">Chi-kwan Chan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davelaar_J/0/1/0/all/0/1">Jordy Davelaar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zanna_L/0/1/0/all/0/1">Luca Del Zanna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Etienne_Z/0/1/0/all/0/1">Zachariah B. Etienne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fragile_P/0/1/0/all/0/1">P. Chris Fragile</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kelly_B/0/1/0/all/0/1">Bernard J. Kelly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liska_M/0/1/0/all/0/1">Matthew Liska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Markoff_S/0/1/0/all/0/1">Sera Markoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKinney_J/0/1/0/all/0/1">Jonathan C. McKinney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mishra_B/0/1/0/all/0/1">Bhupendra Mishra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noble_S/0/1/0/all/0/1">Scott C. Noble</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olivares_H/0/1/0/all/0/1">Héctor Olivares</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prather_B/0/1/0/all/0/1">Ben Prather</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rezzolla_L/0/1/0/all/0/1">Luciano Rezzolla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryan_B/0/1/0/all/0/1">Benjamin R. Ryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_J/0/1/0/all/0/1">James M. Stone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomei_N/0/1/0/all/0/1">Niccolò Tomei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_C/0/1/0/all/0/1">Christopher J. White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Younsi_Z/0/1/0/all/0/1">Ziri Younsi</a>, The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Event_Horizon_Telescope/0/1/0/all/0/1">Event Horizon Telescope Collaboration</a>

Recent developments in compact object astrophysics, especially the discovery
of merging neutron stars by LIGO, the imaging of the black hole in M87 by the
Event Horizon Telescope (EHT) and high precision astrometry of the Galactic
Center at close to the event horizon scale by the GRAVITY experiment motivate
the development of numerical source models that solve the equations of general
relativistic magnetohydrodynamics (GRMHD). Here we compare GRMHD solutions for
the evolution of a magnetized accretion flow where turbulence is promoted by
the magnetorotational instability from a set of nine GRMHD codes: Athena++,
BHAC, Cosmos++, ECHO, H-AMR, iharm3D, HARM-Noble, IllinoisGRMHD and KORAL.
Agreement between the codes improves as resolution increases, as measured by a
consistently applied, specially developed set of code performance metrics. We
conclude that the community of GRMHD codes is mature, capable, and consistent
on these test problems.

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