Microscopic pn-QRPA calculations (without the Brink-Axel hypothesis) of electron-capture and beta-decay rates for the twenty most important fp-shell nuclei with A<65, together with their nuclear mass fractions from Saha's equation under nuclear statistical equilibrium, tabulated across the stellar densities and temperatures of a silicon-burning core. Learners see how the weak rates and abundances that govern the electron-to-baryon ratio of a presupernova star are assembled, and how these microscopic rates differ from large-scale shell-model and independent-particle-model estimates that feed core-collapse supernova simulations.
This nuclear-astrophysics paper (Brazilian Journal of Physics 52:13, 2022) computes the stellar weak-interaction rates (electron capture and beta decay) and the nuclear mass fractions of the twenty m…