Bochum 2009 – wissenschaftliches Programm
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HK: Fachverband Hadronen und Kerne
HK 60: Nuclear Astrophysics
HK 60.3: Vortrag
Mittwoch, 18. März 2009, 17:30–17:45, H-ZO 60
R-process nucleosynthesis calculations with complete nuclear physics input — •Ilka Petermann1,2, Almudena Arcones1,2, Aleksandra Kelic2, Karlheinz Langanke2,1, Gabriel Martinez-Pinedo2, Igor Panov3, Thomas Rauscher3, Karl-Heinz Schmidt2, Friedrich-Karl Thielemann3, and Nikolaj Zinner4 — 1IKP, TU Darmstadt, Germany — 2GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt, Germany — 3Department für Physik und Astronomie, Universität Basel, Switzerland — 4Department of Physics, Harvard University, Cambridge, MA 02138
Elements heavier than iron are known to be made partly by the r-process, 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, but observations indicate at least two possible sites contributing to the solar system abundance of r-process elements and confirm a robust mechanism of the production of elements heavier than Z=56. From the nuclear-physics point of view the r-process requires the knowledge of a large number of reaction rates involving exotic nuclei. We have developed a complete database of reaction rates that besides neutron-capture rates and beta-decay half-lives includes all possible reactions that can induce fission (neutron-capture, beta-decay and spontaneous fission) and the corresponding fission yields. In addition, these reaction rates were implemented in a fully implicit reaction network. We have performed r-process calculations for the neutrino-driven wind scenario to explore whether or not fission can contribute to provide a robust r-process pattern.