Neutrino and antineutrino energy loss rates in massive stars due to isotopes of titanium

TL;DR

This paper calculates neutrino and antineutrino energy loss rates for titanium isotopes in massive stars using pn-QRPA theory, highlighting their significance in stellar evolution and core-collapse modeling.

Contribution

It provides new microscopic calculations of weak rates for titanium isotopes, improving accuracy over previous models and aiding stellar evolution simulations.

Findings

Energy loss rates are over 100 times higher at high temperatures compared to shell model results.

Results suggest stellar cores with lower entropies are favored during late stellar evolution.

Data can improve core-collapse supernova simulations.

Abstract

Weak interaction rates on titanium isotopes are important during the late phases of evolution of massive stars. A search was made for key titanium isotopes from available literature and a microscopic calculation of weak rates of these nuclei were performed using the proton-neutron quasiparticle random phase approximation (pn-QRPA) theory. Earlier the author presented the stellar electron capture rates on titanium isotopes. In this paper I present the neutrino and antineutrino energy loss rates due to capture and decay rates on isotopes of titanium in stellar environment. 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 results are also compared against previous calculations. At high stellar temperatures the calculated neutrino and antineutrino energy loss rates are bigger by more than two orders of magnitude as compared to the large scale shell model results and favor stellar cores with lower entropies. This study can prove useful for core-collapse simulators.