Stellar neutrino energy loss rates due to ${}^{24}$Mg suitable for O+Ne+Mg core simulations

Abstract

Neutrino losses from proto-neutron stars play a pivotal role to decide if these stars would be crushed into black holes or explode as supernovae. Recent observations of subluminous Type II-P supernovae (e.g., 2005cs, 2003gd, 1999br, 1997D) were able to rejuvenate the interest in 8-10 M${}_{\odot }$ stars which develop O+Ne+Mg cores. Simulation results of O+Ne+Mg cores show varying results in converting the collapse into an explosion. The neutrino energy loss rates are important input parameters in core collapse simulations. Proton-neutron quasi-particle random phase approximation (pn-QRPA) theory has been used for calculation of neutrino energy loss rates due to ${}^{24}$Mg in stellar matter. The rates are presented on a detailed density-temperature grid suitable for simulation purposes. The calculated neutrino energy loss rates are enhanced up to more than one order of magnitude compared to the shell model calculations and favor a lower entropy for the core of these massive stars.

20 pages, 4 figures, 2 tables

References in corpus (7)

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• Gamow-Teller transitions and deformation in the proton-neutron random phase approximation
• Comparative study of Gamow-Teller strength distributions in the odd-odd nucleus 50V and its impact on electron capture rates in astrophysical environments
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• Uncertainties in the $0\nu \beta \beta$--decay nuclear matrix elements
• Detailed microscopic calculation of stellar electron and positron capture rates on ${}^{24}$Mg for O+Ne+Mg core simulations

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