Short-lived s-process gamma-ray lines in type II supernovae

Details Short-lived s-process gamma-ray lines in type II supernovae Short-lived s-process gamma-ray lines in type II supernovae

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988sci...240...60h&link_type=abstract

Science (ISSN 0036-8075), vol. 240, April 1, 1988, p. 60-62.

Physics

5

Abundance, Gamma Rays, Helium, Nuclear Fusion, Stellar Mass, Supernovae, Nuclear Reactions, Stellar Envelopes, Stellar Evolution, Stellar Models, Supernova 1987A

Scientific paper

The nuclear abundances in the He-burning shells of presupernova stellar models are calculated. For stars of over 20 solar masses the Ne-22(alpha, n)Mg-25 reaction produces enough neutrons on a sufficiently short time scale for the s-process to produce Fe-59 (half-life = 45 d) and Co-60 (half-life = 5.3 yr). These isotopes are expected to survive the passage of the shock, and gamma rays from their decays should be detectable from most Galactic type II supernovae with the NASA Gamma Ray Observatory. Because of its great distance and low metallicity, these lines are not expected to be observable from supernova 1987A.

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