Background: For the description of many astrophysical processes, precise knowledge of cross sections and reaction rates is necessary. In particular, the exact nucleosynthesis mechanisms of the p nuclei-a group of 30 to 35 neutron deficient nuclei-are still unknown. Since many reactions of astrophysical relevance are not accessible in the laboratory, one has to rely on theoretical calculations based on Hauser-Feshbach codes. The calculated values depend strongly on nuclear physics input parameters like nuclear level densities (NLDs), gamma-ray strength functions (gamma-SFs) and particle+nucleus optical model potentials (OMPs).
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