Massive stars end their life in an explosion event with kinetic energies of the order 1 Bethe. Immediately after the explosion has been launched, a region of low density and high entropy forms behind the ejecta which is continuously subject to neutri
no heating. The neutrinos emitted from the remnant at the center, the protoneutron star (PNS), heat the material above the PNS surface. This heat is partly converted into kinetic energy and the material accelerates to an outflow that is known as the neutrino driven wind. For the first time, we simulate the collapse, bounce, explosion and the neutrino driven wind phases consistently over more than 20 seconds. Our numerical model is based on spherically symmetric general relativistic radiation hydrodynamics using spectral three flavor Boltzmann neutrino transport. In simulations where no explosions are obtained naturally, we model neutrino driven explosions for low and intermediate mass Fe-core progenitor stars by enhancing the charged current reaction rates. In the case of a special progenitor star, the O-Ne-Mg-core, the explosion in spherical symmetry was obtained without enhanced opacities. The post explosion evolution is in qualitative agreement with static steady-state and parametrized dynamic models of the neutrino driven wind. On the other hand, we find generally smaller neutrino luminosities and mean neutrino energies as well as a different evolutionary behavior of the neutrino luminosities and mean neutrino energies. The neutrino driven wind is proton-rich for more than 10 seconds and the contraction of the PNS differs from the assumptions made for the conditions at the inner boundary in previous neutrino driven wind studies. Despite the moderately large entropies per baryon of about 100 and the fast expansion timescale, the conditions found in our model are unlikely to favor...
