Abstract
The weak interaction rates in stellar matter are calculated for the sd-shell nuclei in the full-shell model configurations using the effective interaction of Wildenthal, taking into account the recent extensive compilations of experimental energy levels and Gamow-Teller β decay rates. Based on comparisons between the present calculation and that of Fuller, Fowler, and Newman (FFN), it is pointed out that correct treatment of nuclear structure effects is decisive in attaining reliable weak interaction rates in stellar matter. The weak rates are tabulated at the same grid points of density and temperature as those of FFN, for the ranges 10 ≤ ρYe (g·cm−3) ≤ 1011 and 0.01 × 109 ≤ T (K) ≤ 30 × 109.
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