Abstract :
We study the r-process nucleosynthesis in a prompt supernova explosion and in neutrino-driven winds above proto-neutron stars born in supernova explosions. We perform the numerical simulations of hydrodynamics adopting the relativistic EOS table and the extended nuclear reaction network. We show that successful r-process nucleosynthesis can take place in these two scenarios of r-process in collapse-driven supernovae corresponding to different explosion mechanisms from presupernova stars with different masses. The two scenarios are viable to explain the universal r-process abundance pattern which is found in extremely-metal poor stars and is accord with the solar abundance pattern.
