2010/12/22 by Almudena Arcones, A. Arcones
Physics and Astronomy · #Astronomical and nuclear sciences #Astrophysics #Ejecta #Explosive material #Gamma-ray bursts and supernovae #Neutrino #Neutron #Neutron star #Nuclear physics #Nuclear physics research studies #Nucleosynthesis #Physics #Supernova #Type II supernova #astro-ph.SR #nucl-ex #nucl-th #r-process
paper · pdf · doi:10.1088/1742-6596/312/4/042005
10 pages, 8 figures, invited talk, INPC 2010 Vancouver, Journal of Physics: Conference Series
arxiv created 2010/12/22 · openalex publication_date 2011/09/23 · arxiv updated 2015/05/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The specific mechanism and astrophysical site for the production of half of the elements heavier than iron via rapid neutron capture (r-process) remains to be found. In order to reproduce the abundances of the solar system and of the old halo stars, at least two components are required: the heavy r-process nuclei ( A > 130) and the weak r-process which correspond to the lighter heavy nuclei ( A < 130). In this work, we present nucleosynthesis studies based on trajectories of hydrodynamical simulations for core-collapse supernovae and their subsequent neutrino-driven winds. We show that the weak r-process elements can be produced in neutrino-driven winds and we relate their abundances to the neutrino emission from the nascent neutron star. Based on the latest hydrodynamical simulations, heavy r-process elements cannot be synthesized in the neutrino-driven winds. However, by artificially increasing the wind entropy, elements up to A = 195 can be made. In this way one can mimic the general behavior of an ejecta where the r-process occurs. We use this to study the impact of the nuclear physics input (nuclear masses, neutron capture cross sections, and beta-delayed neutron emission) and of the long-time dynamical evolution on the final abundances.