Neutrino and anti-neutrino energy loss rates due to iron isotopes suitable for core-collapse simulations

TL;DR

This paper presents detailed calculations of neutrino and antineutrino energy loss rates due to iron isotopes, crucial for modeling late stellar evolution stages and supernovae, using an improved microscopic approach.

Contribution

First fine-grid calculation of neutrino energy loss rates for $^{54,55,56}$Fe in stellar matter using pn-QRPA theory, aiding core-collapse simulations.

Findings

Calculated rates differ from previous models, providing more accurate data.

Results are suitable for interpolation in stellar evolution codes.

Comparison shows improvements over earlier calculations.

Abstract

Accurate estimate of neutrino energy loss rates are needed for the study of the late stages of the stellar evolution, in particular for cooling of neutron stars and white dwarfs. The energy spectra of neutrinos and antineutrinos arriving at the Earth can also provide useful information on the primary neutrino fluxes as well as neutrino mixing scenario (it is to be noted that these supernova neutrinos are emitted after the supernova explosion which is a much later stage of stellar evolution than that considered in this paper). Recently an improved microscopic calculation of weak-interaction mediated rates for iron isotopes was introduced using the proton-neutron quasiparticle random phase approximation (pn-QRPA) theory. Here I present for the first time the fine-grid calculation of the neutrino and anti-neutrino energy loss rates due to $^{54,55,56}$Fe in stellar matter. In the core of massive stars isotopes of iron, $^{54,55,56}$Fe, are considered to be key players in decreasing the electron-to-baryon ratio ($Y_{e}$) mainly via electron capture on these nuclide. Core-collapse simulators may find this calculation suitable for interpolation purposes and for necessary incorporation in the stellar evolution codes. The calculated cooling rates are also compared with previous calculations.