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By R-process Nucleosynthesis, I. Petermann, A. Arcones and G. Martínez-pinedo

Abstract

Elements heavier than iron are known to be made partly by the r-process, in a sequence of rapid neutron-captures and subsequent beta-decays in explosive scenarios with high neutron densities. Its astrophysical site has not yet been identified, despite the numerous works done in the last 50 years (see [2] for a review). We have studied systematically the nucleosynthesis production in neutrino-driven winds and analyzed the influence of different factors like the nuclear physics input and fission. Trajectories from long time supernova simulations ([1]) have been used as input in an explicit nuclear reaction network, which includes neutron capture, photodissociation, beta decay and fission. The conditions found in the supernova simulations (too low entropy and /or electron fraction) do not result in large enough neutron-to-seed ratio to produce elements heavier than A≈70. However by increasing slightly the entropy the neutron-to-seed ratio is large enough to produce r-process nuclei reaching A≈195. We have used the resulting trajectories to analyze the combined effect of uncertainties in the nuclear and astrophysical inputs. The later one includes the influence that the reverse shock may have in the matter expansion velocity. We have performed nucleosynthesis calculations using four different mass models (FRDM, ETFSI-Q, HFB-14, Duflo Zuker) for which we have computed the relevant neutroncapture rates. The impact that the different mass models have in the final abundances is shown in Fig. 1. abundanc

Year: 2010
OAI identifier: oai:CiteSeerX.psu:10.1.1.161.8520
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