The p-process in SN 1987 A

Details The p-process in SN 1987 A The p-process in SN 1987 A

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...238..455p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 238, no. 1-2, Nov. 1990, p. 455-461. Research supported by EEC.

Astronomy and Astrophysics

Astrophysics

65

Nuclear Fusion, Nuclear Reactions, Solar System, Supernova 1987A, Abundance, Hydrodynamic Equations, Stellar Models

Scientific paper

The nucleosynthesis of the proton-rich isotopes is studied in a realistic model for the type II supernova SN 1987 A. The presupernova model consists of an evolved 6 solar mass helium star in which a O/Ne-rich zone is selected containing 18 different layers heated during the explosion to peak temperatures ranging from 1.98 to 3.30 billion K. These temperatures, as well as the time variation of temperature and density in these layers have been obtained from hydrodynamical calculations. The seed nuclei abundances are derived from an s-process occurring during the core He-burning phase of the supernova progenitor. The p-nuclei synthesis is calculated with an extended reaction network using state-of-the-art nuclear rates. The resulting p-nuclei abundance pattern averaged over the whole stellar zone compares to the solar one to within a factor three for about 50 percent of the p-nuclei. The overproduction factors obtained as a function of peak temperature are discussed, and the sensitivity of these factors to the detailed physical conditions is emphasized. The rare isotope ta-180 appears for the first time to be significantly produced in a p-process calculation.

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