Proto-neutron star evolution with improved charged-current neutrino–nucleon interactions

We perform simulations of the Kelvin-Helmholtz cooling phase proto-neutron stars with a new numerical code in spherical symmetry and using quasi-static approximation. use for first time full set charged-current neutrino-nucleon reactions, including neutron decay modified Urca processes, together energy-dependent representation inclusion nuclear correlations random-phase Moreover, convective motions are taken into account within mixing-length theory. As we vary assumptions computing reaction rates, show that dominant effect on timescale, neutrino signal composition neutrino-driven wind comes from motion. Computation random approximation, as compared to mean field approach, has relatively small impact.