General-Relativistic Large-Eddy Simulations of Binary Neutron Star Mergers

摘要: The flow inside remnants of binary neutron star (NS) mergers is expected to be turbulent, because magnetohydrodynamics instability activated at scales too small resolved in simulations. To study the large-scale impact these instabilities, we develop a new formalism, based on large-eddy simulation technique, for modeling subgrid-scale turbulent transport general relativity. We apply it, first time, late-inspiral and merger two NSs. find that turbulence can significantly affect structure survival time remnant, as well its gravitational-wave (GW) neutrino emissions. former will relevant GW observation merging stars. latter composition outflow driven by might influence nucleosynthetic yields. accretion rate after black-hole formation also affected. Nevertheless, that, most likely values mixing efficiency, effects are relatively signal affected only weakly turbulence. Thus, our simulations provide validation all existing post-merger models.