Possibility of synthesis of proton-rich nuclei in highly evolved stars. II

Details Possibility of synthesis of proton-rich nuclei in highly evolved stars. II Possibility of synthesis of proton-rich nuclei in highly evolved stars. II

Jan 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....46..117a&link_type=abstract

Astronomy and Astrophysics, vol. 46, no. 1, Jan. 1976, p. 117-125. Research supported by the Fonds National Belge de la Recherc

Astronomy and Astrophysics

Astrophysics

48

Abundance, Astronomical Models, Nuclear Fusion, Protons, Stellar Evolution, Interstellar Matter, Neutrinos, Solar System

Scientific paper

Exploratory calculations performed to examine the possibility of production of p-elements in conditions which might be typical of certain hydrostatic oxygen burning phases are presented. Temperature, density and neutron concentration are assumed to be constant in time and some enhancement of the seed r and/or s-nuclei is assumed with respect to the solar abundances. In such conditions, a great number of p-elements might be overproduced in ratios close to their solar values if a superposition of at least three abundance distributions corresponding to somewhat different temperatures (2-2.2 billion K), neutron concentrations (.01 to 1.0 quadrillion/cu cm), and eventually time scales. These distributions are meant to account for the p-elements in the three mass number ranges 0 to 98, 102-about 144, and about 144 to 196; the agreement between theoretical and observed abundances is the worst for the first of these three classes. Preliminary calculations suggest that it might be worthwhile to reexamine the p-element production problem in the framework of more sophisticated models. The transport of the p-nuclei from the zones of production into the interstellar medium at the right time without any further significant nuclear processing constitutes one of the major difficulties of the model.

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