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}
}
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… 

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