Shell-model calculations of stellar weak interaction rates: II. Weak rates for nuclei in the mass range A=45-65 in supernovae environment

Abstract

Based on large-scale shell model calculations we have determined the electron capture, positron capture and beta-decay rates on more than 100 nuclei in the mass range A=45-65. The rates are given for densities ρY_e =10^7-10^{10} mol/cm^3 and temperatures T=10^9-10^{10} K and hence are relevant for both types of supernovae (Type Ia and Type II). The shell model electron capture rates are significantly smaller than currently assumed. For proton-to-baryon ratios Y_e=0.42-0.46 mol/g, the beta-decay rates are faster than the electron capture rates during the core collapse of a massive star.

16 pages, 10 figures

References in corpus (1)

• Nucleosynthesis in Chandrasekhar Mass Models for Type Ia Supernovae and Constraints on Progenitor Systems and Burning-Front Propagation

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• Electron capture and \b{eta}-decay rates for nuclei with A=65-80
• Magnetic dynamos in white dwarfs -III: explaining the occurrence of strong magnetic fields in close double white dwarfs
• And Don't Forget The Black Holes
• Convective Penetration in Early-Type Stars
• Comprehensive neutrino light curves and spectra: from pre-supernova evolution to early supernova phase
• Calcium Excess in Novae: Beyond Nuclear Physics Uncertainties
• Discerning internal conditions of pulsating hot subdwarf B stars. Modelling multiple trapped modes in KIC 10001893