This document summarizes a study on nucleosynthesis in massive stars using improved nuclear physics and stellar models. The authors present calculations for Pop I stars with masses of 15, 19, 20, 21, and 25 solar masses using updated nuclear reaction rates, opacity tables, neutrino losses, and weak interaction rates. They employ a novel adaptive reaction network of up to 2,200 nuclei to follow nucleosynthesis from hydrogen through polonium. The results show generally good agreement with solar abundances for nuclei from oxygen to zinc. However, discrepancies are found for some isotopes in the 20 solar mass model due to merging of convective shells prior to collapse. The calculations also reveal deficiencies in producing the p-process isotopes of rut

T. Rauscher - Nucleosynthesis in Massive Stars W Improved Physics (LG Article) (2002) PDF

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