The p-process revisited

Details The p-process revisited The p-process revisited

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...227..271r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 227, no. 1, Jan. 1990, p. 271-281. Research supported by FNRS and CNRS.

Astronomy and Astrophysics

Astrophysics

74

Nuclear Astrophysics, Solar System, Stellar Evolution, Supernovae, Abundance, Density Distribution, Nuclear Fusion, Oxygen, Stellar Composition, Stellar Cores, Stellar Temperature

Scientific paper

A parameterized explosion model is used to reinvestigate the synthesis of p-nuclei in the oxygen burning layers of massive exploding stars. Improved nuclear reaction rates and an extended reaction network are used. The latter includes elements between carbon and bismuth and treats self-consistently the neutron, proton and alpha-particle production and captures. Starting with a seed nuclei distribution resulting from an s-process in the helium burning core of a massive star, a p-nuclei abundance pattern is obtained which compares to the solar one within a factor 3 for 60 percent of the p-nuclei. Further test calculations are performed in order to study the effects on the p-process yields of neutron-induced reactions, as well as of the expansion time scale characterizing the explosion. The underproduction of Mo-92, Mo-94, and Ru-96 observed in earlier works, remains in the calculations. A few other nuclides which are classically considered as p-nuclei are also synthesized in insufficient amounts, and an s-process origin for these nuclei is discussed.

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