Neutrino-driven winds and nucleosynthesis

Abstract

Baryonic outflows from proto-neutron stars formed in core-collapse supernova explosions are one of the possible scenarios for the production of heavy elements via the r-process. If the ejected matter reaches supersonic velocities the outflow is known as neutrino-driven wind. We have studied the long-time evolution of proto-neutron stars with one- and two-dimensional hydrodynamical simulations and performed nucleosynthesis calculations with the resulting wind trajectories. We find that the present wind models are much closer than previous studies to provide suitable conditions for r-process nucleosynthesis. Moreover, we explored the effect of the wind terminations shock, nuclear physics input, and composition of the outer layers of the neutron star on the nucleosynthesis production.

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