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

Journal Article · Wed Oct 15 04:00:00 EDT 2008 · Physical Review. C, Nuclear Physics

DOI:https://doi.org/10.1103/PHYSREVC.78.045801· OSTI ID:21192349

Nabi, Jameel-Un ^[1]

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1. Faculty of Engineering Sciences, GIK Institute of Engineering Sciences and Technology, Topi 23640, Swabi, NWFP (Pakistan)

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{sub {center_dot}} stars that 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 quasiparticle random-phase approximation (pn-QRPA) theory has been used for calculation of neutrino energy loss rates due to {sup 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.

• OSTI ID: 21192349
• Journal Information: Physical Review. C, Nuclear Physics, Journal Name: Physical Review. C, Nuclear Physics Journal Issue: 4 Vol. 78; ISSN 0556-2813; ISSN PRVCAN
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
BLACK HOLES
DENSITY
ENERGY LOSSES
ENTROPY
EXPLOSIONS
MAGNESIUM
MAGNESIUM 24
NEON
NEUTRINOS
NEUTRON STARS
NEUTRONS
OXYGEN
PROTONS
RANDOM PHASE APPROXIMATION
SHELL MODELS
SIMULATION
SUPERNOVAE