Seed abundances for r-processing in the helium shells of supernovae

Details Seed abundances for r-processing in the helium shells of supernovae Seed abundances for r-processing in the helium shells of supernovae

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...241.1090c&link_type=abstract

Astrophysical Journal, Part 1, vol. 241, Nov. 1, 1980, p. 1090-1093.

Astronomy and Astrophysics

Astrophysics

21

Abundance, Helium, Nuclear Fusion, Stellar Envelopes, Supernovae, Heavy Elements, Shock Heating, Stellar Evolution

Scientific paper

The production of r-process nuclei as a consequence of shock heating of the helium shells in supernovae is examined. The assumption of an initial (seed) distribution which is enriched in heavy s-process elements relative to solar system matter is found to allow production of r-process abundance features compatible with observations. Such an enrichment is consistent, for example, with the high Ba/Sr ratios characteristic of barium stars. This may result from the mixing of hydrogen-rich matter into the helium shells during earlier phases of stellar evolution. With such enrichments, the production of r-process nuclei in solar proportions in the helium shells of supernovae (the 'helium' driven r-process) becomes possible.

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