Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear matrix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem

Details Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear matrix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear matrix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem

Mar 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apjs...42..447f&link_type=abstract

Astrophysical Journal Supplement Series, vol. 42, Mar. 1980, p. 447-473.

Astronomy and Astrophysics

Astrophysics

177

Neutrinos, Nuclear Astrophysics, Nuclear Reactions, Supernovae, Weak Interactions (Field Theory), Aluminum 26, Electron Capture, Electron Transitions, Energy Dissipation, Positrons, Reaction Kinetics

Scientific paper

Astrophysical positron emission, continuum electron capture, and neutrino energy loss rates are calculated for 26Al → 26Mg, 30P → 30Si;, 31S → 31P, 32S → 32P 33S → 33P, and 35Cl → 35S. Measured nuclear level information and matrix elements are used where available. Unmeasured matrix elements for allowed transitions are assigned on the basis of simple shell model arguments and the results of detailed large-scale shell model calculations by Wildenthal and his collaborators. The experimentally determined matrix elements are found to dominate the rates over most of the range of temperatures and densities considered. The uncertainties in the rates are estimated. Appropriate average matrix elements for unmeasured Gamow-Teller transitions are estimated for use in other sd-shell nuclei. The rates presented agree roughly with those of Hansen over a wide range of conditions, but potentially important differences in the rates exist at temperatures and densities relevant for the production and destruction of 26Al and for neutronization and neutrino loss in the late stages of presupernova evolution.

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