$nutexttt{bhlight}$: Radiation GRMHD for Neutrino-Driven Accretion Flows. (arXiv:1903.09273v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">Jonah M. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryan_B/0/1/0/all/0/1">Ben R. Ryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dolence_J/0/1/0/all/0/1">Joshua C. Dolence</a>

The 2017 detection of the in-spiral and merger of two neutron stars was a
landmark discovery in astrophysics. We now know that such mergers are central
engines of short gamma ray bursts and sites of r-process nucleosynthesis, where
the heaviest elements in our universe are formed. In the coming years, we
expect many more such mergers. Modeling such systems presents a significant
computational challenge along with the observational one. To meet this
challenge, we present $nutexttt{bhlight}$, a scheme for solving general
relativistic magnetohydrodynamics with energy-dependent neutrino transport in
full (3+1)-dimensions, facilitated by Monte Carlo methods. We present a suite
of tests demonstrating the accuracy, efficacy, and necessity of our scheme. We
demonstrate the potential of our scheme by running a sample calculation in a
domain of interest—the dynamics and composition of the accretion disk formed
by a binary neutron star merger.

The 2017 detection of the in-spiral and merger of two neutron stars was a
landmark discovery in astrophysics. We now know that such mergers are central
engines of short gamma ray bursts and sites of r-process nucleosynthesis, where
the heaviest elements in our universe are formed. In the coming years, we
expect many more such mergers. Modeling such systems presents a significant
computational challenge along with the observational one. To meet this
challenge, we present $nutexttt{bhlight}$, a scheme for solving general
relativistic magnetohydrodynamics with energy-dependent neutrino transport in
full (3+1)-dimensions, facilitated by Monte Carlo methods. We present a suite
of tests demonstrating the accuracy, efficacy, and necessity of our scheme. We
demonstrate the potential of our scheme by running a sample calculation in a
domain of interest—the dynamics and composition of the accretion disk formed
by a binary neutron star merger.

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