The Accretion Phase of Core Collapse Supernovae

We present data from recent core collapse simulations, using spherically symmetric general relativistic radiation hydrodynamics featuring a three-flavor neutrino Boltzmann transport solver and an equation of state (eos) for hot and dense nuclear matter. A nuclear reaction network has recently been implemented, which allows us to investigate explosion models into the neutrino wind phase several seconds after core bounce. In the absence of an earlier explosion, the continuous accretion of outer layers of the progenitor star lead eventually to the collapse of the protoneutron star (PNS) at the very center and the formation of a black hole.