Electron capture rates for core collapse supernovae

Abstract

Electron capture rates on neutron-rich nuclei (A>65) were calculated within the Random Phase Approximation with partial number formalism, including allowed and forbidden transitions. The partial occupation numbers were provided as a function of temperature by Shell-Model Monte Carlo calculations, including an pairing+quadrupole interaction. Capture rates on relevent nuclei were calculated for density and temperature conditions during the core collapse of a massive star. It was found that electron captures on nuclei can compete with electron captures on free protons. Furthermore, they produce neutrinos with average energies lower than neutrinos emitted from captures on free protons, with possible consequences on the cooling of the core.

3 pages, 4 figures, submitted to the proceedings of Nuclei in the Cosmos XVII

References in corpus (1)

• Unblocking of the Gamow-Teller strength in stellar electron capture on neutron-rich Germanium isotopes

Cited by in corpus (4)

• Improved estimate of electron capture rates on nuclei during stellar core collapse
• Nuclear weak interaction rates in primordial nucleosynthesis
• Study of Gamow-Teller strength and associated weak-rates on odd-A nuclei in stellar matter
• Investigation of weak-rates for odd-A nuclei for presupernova simulations