Journal
ASTROPHYSICAL JOURNAL
Volume 919, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac1119
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Funding
- Heising-Simons Foundation
- Danish National Research Foundation [DNRF132]
- NSF [PHY-2012057, AST-1909534, AST-1911206, AST-1852393]
- UCMEXUS-CONACYT Doctoral Fellowship
- NASA Goddard Center for Research and Exploration in Space Science and Technology (CRESST) II Cooperative Agreement [80GSFC17M0002]
- NASA TCAN award [TCAN-80NSSC18K1488]
- NSF MRI grant [AST 1828315]
- TACC's Frontera NSF project [PHY20010, AST20021]
- NCSA's Blue Waters sustained-petascale computing NSF project [OAC-1811228, OAC-1516125]
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Researchers are working on simulating and testing finite-temperature EOS and neutrino treatment in GRMHD code to understand the physical processes in post-merger disks of neutron star mergers.
The first binary neutron star merger has already been detected in gravitational waves. The signal was accompanied by an electromagnetic counterpart including a kilonova component powered by the decay of radioactive nuclei, as well as a short gamma-ray burst. In order to understand the radioactively powered signal, it is necessary to simulate the outflows and their nucleosynthesis from the post-merger disk. Simulating the disk and predicting the composition of the outflows requires general relativistic magnetohydrodynamical (GRMHD) simulations that include a realistic, finite-temperature equation of state (EOS) and self-consistently calculating the impact of neutrinos. In this work, we detail the implementation of a finite-temperature EOS and the treatment of neutrinos in the GRMHD code HARM3D+NUC, based on HARM3D. We include formal tests of both the finite-temperature EOS and the neutrino-leakage scheme. We further test the code by showing that, given conditions similar to those of published remnant disks following neutron star mergers, it reproduces both recombination of free nucleons to a neutron-rich composition and excitation of a thermal wind.
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