Relativistic Neutrino Transport in Stellar Collapse

Abstract

In stellar core collapse, the initial bounce shock energy derives from core compression almost high enough to form an event horizon and black hole. We are interested in maximizing this compression in order to make a strong supernova explosion and also in collapses that, after emitting an observable neutrino signal, accrete enough matter to form a black hole rather than remnant neutron star. We have therefore developed a neutrino radiation hydrodynamics [1,2,4 that gives complete coverage of the space-time domain of outer communication as seen by a distant observer.