Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars
arXiv:2504.14197 · doi:10.1016/j.newast.2019.03.001
Abstract
Simulation studies indicate that weak interaction rates on nickel isotopes play a crucial role in determining the electron-to-baryon ratio within the stellar interior during the late stages of core evolution. (Anti)neutrinos produced through weak decay processes escape from stellar regions with densities below 10^11 g/cm^3, carrying away energy and thereby reducing the core entropy. In this work, we present a microscopic calculation of neutrino and antineutrino cooling rates resulting from weak interactions on nickel isotopes in the mass range 56 <= A <= 71. The calculations are performed using the deformed proton-neutron Quasiparticle Random Phase Approximation (pn-QRPA) model. Recent investigations into the Gamow-Teller (GT) strength distributions of nickel isotopes demonstrate that the deformed pn-QRPA model successfully reproduces experimental charge-changing transition data.
arXiv comment33 pages, 8 tables, 9 figures
References in corpus (24)
- Nuclear Ground-State Masses and Deformations
- Theory of Core-Collapse Supernovae
- Shell-model calculations of stellar weak interaction rates: II. Weak rates for nuclei in the mass range A=45-65 in supernovae environment
- Nuclear weak-interaction processes in stars
- Superallowed 0+ to 0+ nuclear beta decays: A new survey with precision tests of the conserved vector current hypothesis and the standard model
- Core-Collapse Simulations of Rotating Stars
- Neutrino-driven supernova of a low-mass iron-core progenitor boosted by three-dimensional turbulent convection
- Presupernova Evolution with Improved Rates for Weak Interactions
- Presupernova collapse models with improved weak-interaction rates
- Dynamics of shock propagation and nucleosynthesis conditions in O-Ne-Mg core supernovae
- Weak Interaction Rates Of sd-Shell Nuclei In Stellar Environment Calculated in the Proton-Neutron Quasiparticle Random Phase Approximation
- Estimates of Stellar Weak Interaction Rates for Nuclei in the Mass Range A=65-80
- General Relativistic Effects in the Core Collapse Supernova Mechanism
- Microscopic Calculations of Weak Interaction Rates of Nuclei in Stellar Environment for A = 18 to 100
- Modification of the Brink-Axel Hypothesis for High Temperature Nuclear Weak Interactions
- Gamow-Teller strength distributions and electron capture rates for 55Co and 56Ni
- Systematics of strength function sum rules
- Comparative study of Gamow-Teller strength distributions in the odd-odd nucleus 50V and its impact on electron capture rates in astrophysical environments
- Nickel isotopes in stellar matter
- Unique first-forbidden -decay transitions in odd-odd and even-even heavy nuclei
- Stellar neutrino energy loss rates due to Mg suitable for O+Ne+Mg core simulations
- Investigation of Gamow Teller Transition Properties in 56-64Ni Isotopes Using QRPA Methods
- Gamow-Teller strength and lepton captures rates on 66-71Ni in stellar matter
- Allowed and unique first-forbidden stellar electron emission rates of neutron-rich copper isotopes