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

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.

16 pages, 7 figures

References in corpus (4)

• Comparative study of Gamow-Teller strength distributions in the odd-odd nucleus 50V and its impact on electron capture rates in astrophysical environments
• Weak-interaction mediated rates on iron isotopes for presupernova evolution of massive stars
• Uncertainties in the $0\nu \beta \beta$--decay nuclear matrix elements
• Neutrino energy loss rates and positron capture rates on ${}^{55}$Co for presupernova and supernova physics

Cited by in corpus (2)

• Ground and excited states Gamow-Teller strength distributions of iron isotopes and associated capture rates for core-collapse simulations
• Energy Rates Due to Weak Decay Rates of Vanadium Isotopes in Stellar Environment