Neutrinos in Generic Binary Neutron Stars Configurations
In this work we implement improvements in the BAM code for simulations of astrophysical systems in the context of Numerical Relativity. Such enhancements consist of the introduction of the computational infrastructure necessary for the use of equations of state (EoSs) derived from microscopic theories to realistically describe stellar matter in high density, finite temperature regimes. Furthermore, weak interaction mechanisms driven by neutrinos are considered through the so-called Neutrinos Leakage Scheme (NLS) and the M1 formalism for the radiation transport equations. At the present stage we present TOV star simulations performed in order to successfully reproduce results from the literature that suggest the occurrence of neutrinos-induced gravitational collapse as of the NLS in configurations initially belonging to the unstable branch of central densities. This result serves as a testbed for the new features now considered. We also perform binary neutron star (BNS) late inspiral, merger and post-merger simulations using the new numerical tooling implemented in this work in order to validate our methods by comparing the outcomes with results reported in the literature. Finally, radiation transport simulations with the M1 scheme were performed in physical situations of interest in order to assess the degree of success achieved by our code.