Speaker: Toshihiko Kawano (T-16, LANL)

Neutron capture calculations for astrophysics

Nuclear reaction process for astrophysics applications is discussed. The most important reaction process for nucleosynthesis is the neutron capture, and the capture rate can be calculated with the statistical Hauser-Feshbach model with width fluctuation correction. The HF model like GNASH has been widely used for calculations of nuclear reaction cross sections, and in many cases this model gives a satisfactory fit to experimental data available at low energies. For the r-process, we need to calculate the capture cross sections up to several MeV, so that the Direct/Semidirect (DSD) model calculations are also needed. The calculated capture cross sections for Zr isotopes are shown, and systematics of model parameters are discussed.

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