The p-process in supernovae

Details The p-process in supernovae The p-process in supernovae

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apjs...36..285w&link_type=abstract

Astrophysical Journal Supplement Series, vol. 36, Feb. 1978, p. 285-304.

Physics

Nuclear Physics

150

Abundance, Nuclear Fusion, Supernovae, Atomic Weights, Disintegration, Heavy Elements, Isotopes, Nuclei (Nuclear Physics), Proton Flux Density, Stellar Evolution, Stellar Structure, Tables (Data), Temperature Distribution

Scientific paper

The nucleosynthetic origin of the rare proton-rich isotopes, usually called 'p-process' isotopes, is examined. A particularly interesting context for this synthesis is found to be explosive events characterized by peak temperatures in the range from 2 to 3 billion K. At these temperatures a series of photodisintegration reactions operating upon a distribution of r- and s-process seeds produces an abundance pattern that displays striking similarities to that of the p-process nuclei in the solar system. The large proton densities usually required for such synthesis are not needed. Requisite conditions for this model are expected to occur naturally in those zones of supernovae that have experienced helium and perhaps carbon burning prior to explosion. Implications for supernova structure, presupernova evolution, and cosmochronology are discussed, and a critical discussion of other current p-process models is presented.

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