出版社:SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要: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.