Abstract
We present recent progress of our studies on r-process nucleosynthesis in collapse-driven supernovae based on the physics of unstable nuclei in the light of astronomical observations. We have studied r-process in prompt explosions and in neutrino-driven winds by hydrodynamical simulations with the relativistic EOS table and the extended nuclear reaction network. We have found that successful r-process, which explains the solar abundance pattern, can occur in the neutron-rich material ejected from prompt explosions and in the neutrino-driven winds with short expansion time scale. These findings suggest that the r-process in supernovae is closely related with the explosion mechanism and the r-process abundance pattern may depend on the mass range of presupernova stars. Two scenarios might explain well the recent detections of r-process elements in extremely metal-poor stars as well as systematics by future observations.
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