• DOI:10.1086/190657
• Corpus ID: 122110982

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

@article{Fuller1980StellarWR,
  title={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},
  author={George M. Fuller and William A. Fowler and M. J. Newman},
  journal={Astrophysical Journal Supplement Series},
  year={1980},
  volume={42},
  pages={447-473}
}

• G. Fuller, W. Fowler, M. Newman
• Published 1 March 1980
• Physics
• Astrophysical Journal Supplement Series

Astrophysical positron emission, continuum electron capture, and neutrino energy loss rates are calculated for 26 A1—> 26 Mg, 30 P—» 30 Si, 31 S—> 31 P, 32 S—> 32 P, 33 S-> 33 P, and 35 C1-* 35 S. 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 ¿¿/-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 26 A1 and for neutronization and neutrino loss in the late stages of presupemova evolution.