Neutrino absorption by hot nuclei in supernova environments

Abstract

Using the thermal quasiparticle random phase approximation, we study the process of neutrino and antineutrino capture on hot nuclei in supernova environments. For the sample nuclei ${}^{56}$Fe and ${}^{82}$Ge we perform a detailed analysis of thermal effects on the strength distribution of allowed Gamow-Teller transitions which dominate low-energy charged-current neutrino reactions. The finite temperature cross sections are calculated taking into account the contributions of both allowed and forbidden transitions. The enhancement of the low-energy cross sections is explained by considering thermal effects on the GT${}_{\pm }$ strength. For ${}^{56}$Fe we compare the calculated finite-temperature cross sections with those obtained from large-scale shell-model calculations.

Minor revisions according to referee's recomendations

References in corpus (4)

• Theory of Core-Collapse Supernovae
• Stellar electron-capture rates calculated with the finite-temperature relativistic random-phase approximation
• Neutrino beams as a probe of the nuclear isospin and spin-isospin excitations
• Inelastic neutrino scattering off hot nuclei in supernova environments

Cited by in corpus (9)

• Electron capture in stars
• Temperature dependence of nuclear spin-isospin response and beta decay in hot astrophysical environments
• Impact of complex many-body correlations on electron capture in thermally excited nuclei around ${}^{78}$Ni
• Thermal quasiparticle random-phase approximation calculations of stellar electron capture rates with the Skyrme effective interaction
• Nuclear neutrino energy spectra in high temperature astrophysical environments
• The Skyrme-TQRPA calculations of electron capture on hot nuclei in pre-supernova environment
• Temperature evolution of the nuclear shell structure and the dynamical nucleon effective mass
• Nuclear Weak Rates and Detailed Balance in Stellar Conditions
• Neutrino spectrum and energy loss rates due to weak processes on hot ${}^{56}$Fe in pre-supernova environment