Neutrino energy loss rates and positron capture rates on $^{55}$Co for presupernova and supernova physics

Details Neutrino energy loss rates and positron capture rates on $^{55}$Co for presupernova and supernova physics Neutrino energy loss rates and positron capture rates on $^{55}$Co for presupernova and supernova physics

2011-08-03

arxiv.org/abs/1108.0826v1

Phys.Rev.C77:055802,2008

Physics

Nuclear Physics

Nuclear Theory

27 pages, 6 figures, 5 tables

Scientific paper

10.1103/PhysRevC.77.055802

Proton-neutron quasi-particle random phase approximation (pn-QRPA) theory has recently being used for calculation of stellar weak interaction rates of $fp$-shell nuclide with success. 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. The product of abundance and positron capture rates on $^{55}$Co is substantial and as such can play a role in fine tuning of input parameters of simulation codes specially in the presupernova evolution. Recently we introduced our calculation of capture rates on $^{55}$Co, in a luxurious model space of $7 \hbar \omega$, employing the pn-QRPA theory with a separable interaction. Simulators, however, may require these rates on a fine scale. Here we present for the first time an expanded calculation of the neutrino energy loss rates and positron capture rates on $^{55}$Co on an extensive temperature-density scale. These type of scale is appropriate for interpolation purposes and of greater utility for simulation codes. The pn-QRPA calculated neutrino energy loss rates are enhanced roughly up to two orders of magnitude compared with the large-scale shell model calculations and favor a lower entropy for the core of massive stars.

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