Stellar weak interaction rates for intermediate mass nuclei. III. Rate tables for the free nucleons and nuclei with A = 21 TO A = 60
@article{Fuller1982StellarWI, title={Stellar weak interaction rates for intermediate mass nuclei. III. Rate tables for the free nucleons and nuclei with A = 21 TO A = 60}, author={George M. Fuller and William A. Fowler and M. J. Newman}, journal={Astrophysical Journal Supplement Series}, year={1982}, volume={48}, pages={279-319} }
Stellar electron and positron emission rates and continuum electron and positron capture rates, as well as the associated neutrino energy loss rates, are tabulated for the free nucleons and 226 nuclei with masses between A = 21 and 60. These rates were calculated in accordance with the procedure described in Papers I and II of this series and are presented here in tabular form on an abbreviated temperature and density grid. Results of these calculations on a detailed temperature and density…
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References
preparation. Note added in proof.—We have neglected changes in Qn due to Coulomb plasma effects. In the plasma a nucleus
- Nucl. Phys.,
- 1975