Implications of the recent 59Co(n,p)59Fe experiment for stellar electron capture rates

Details Implications of the recent 59Co(n,p)59Fe experiment for stellar electron capture rates Implications of the recent 59Co(n,p)59Fe experiment for stellar electron capture rates

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phrvc..47.2961a&link_type=abstract

Physical Review C (Nuclear Physics), Volume 47, Issue 6, June 1993, pp.2961-2969

Physics

Nuclear Physics

20

Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Inelastic Neutron Scattering, Beta Decay, Double Beta Decay, Electron And Muon Capture, Shell Model

Scientific paper

We study results from the recent measurement of the 0° 59Co(n,p)59Fe cross section in order to compute the stellar electron capture rate of 59Co. This nucleus is the second most important electron capture nucleus in the core of a type II supernova progenitor just before core collapse. It is also the first nucleus which has a large effect on the stellar neutronization rate for which Gamow-Teller strength has been measured. The Gamow-Teller resonance has been observed experimentally at a higher energy above the daughter ground state than one would expect from independent particle shell model arguments, but large-basis shell model calculations employing configuration mixing are more successful in predicting the location of the strength. Because of the high energy of the Gamow-Teller resonance, the stellar electron capture rate and associated neutronization is much less than previous estimates had indicated. Similar trends are seen for 60Co, the most important electron capture nucleus for supernova progenitors just before core collapse.

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