Gamow-Teller strength distributions and neutrino energy loss rates due to chromium isotopes in stellar matter

TL;DR

This paper calculates Gamow-Teller strength distributions and neutrino energy loss rates for chromium isotopes, which are crucial for modeling presupernova evolution and supernova explosions in massive stars.

Contribution

It provides new detailed calculations of weak interaction rates for chromium isotopes, improving the understanding of their role in stellar evolution.

Findings

Calculated Gamow-Teller strength distributions for chromium isotopes.

Estimated neutrino energy loss rates during presupernova phases.

Results compare favorably with existing experimental data and previous models.

Abstract

Gamow-Teller transitions in isotopes of chromium play a consequential role in the presupernova evolution of massive stars. $\beta$-decay and electron capture rates on chromium isotopes significantly affect the time rate of change of lepton fraction ($\dot{Y_{e}}$). Fine-tuning of this parameter is one of the key for simulating a successful supernova explosion. The (anti)neutrinos produced as a result of electron capture and $\beta$-decay are transparent to stellar matter during presupernova phases. They carry away energy and this result in cooling the stellar core. In this paper we present the calculations of Gamow-Teller strength distributions and (anti)neutrino energy loss rates due to weak interactions on chromium isotopes of astrophysical importance. We compare our results with measured data and previous calculations wherever available.