Münster 2011 – scientific programme

Parts | Days | Selection | Search | Updates | Downloads | Help

HK: Fachverband Physik der Hadronen und Kerne

HK 34: Nukleare Astrophysik - Poster

HK 34.1: Poster

Wednesday, March 23, 2011, 14:00–16:00, Foyer Chemie

Simulation of p-process abundances in supernova explosions — •Jens Ebert¹, Iris Dillmann^1,2, Janos Farkas³, and Zsolt Fülöp³ — ¹Justus-Liebig-Universität Gießen — ²GSI Darmstadt — ³ATOMKI Debrecen

The nucleosynthesis of elements beyond iron is mainly given by neutron capture reactions in s- and r-processes. However 32 stable, proton-rich isotopes between ⁷⁴Se and ¹⁹⁶Hg cannot be produced in that way. These isotopes are accounted to the "p-process", which is in nowadays understanding a superposition of several sub-processes. We have simulated the production of these isotopes from existing s-process seed nuclei via photodisintegration and β⁺-decay ("γ-process") with updated experimental reaction rates from [1] KADoNiS (Karlsruhe Astrophysical Database of Nucleosynthesis in Stars) and the JINA reaction library [1,2].

[1]I. Dillmann, J. Ebert, et al., "Stellar (n,γ) cross sections of p-process isotopes - Part 3: Simulation with an updated reaction library"; Phys. Rev. C (in preparation)

[2]I. Dillmann et al., J. Phys. - G: Nucl. Part. Phys. 35 (2008) 014029