Stellar electron-capture rates in pf-shell nuclei from quasiparticle random-phase approximation calculations

2013/04/08 by P. Sarriguren · 2 citations
Physics and Astronomy · #nucl-th #astro-ph.SR

paper · pdf · doi:10.1103/physrevc.87.045801

published as Physical Review C 87, 045801 (2013) · 18 pages, 26 figures. arXiv admin note: text overlap with arXiv:1102.0628

arxiv created 2013/04/08 · arxiv updated 2013/04/09

Abstract

Electron-capture rates at different density and temperature conditions are evaluated for a set of pf-shell nuclei representative of the constituents in presupernova formations. The nuclear structure part of the problem is described within a quasiparticle random-phase approximation based on a deformed Skyrme Hartree-Fock selfconsistent mean field with pairing correlations and residual interactions in particle-hole and particle-particle channels. The energy distributions of the Gamow-Teller strength are evaluated and compared to benchmark shell-model calculations and experimental data extracted from charge-exchange reactions. The model dependence of the weak rates are discussed and the various sensitivities to both density and temperature are analyzed.

Citations

• Stellar weak decay rates in neutron-deficient medium-mass nuclei

Cited by

• Contribution of excited states to stellar weak-interaction rates in odd-A nuclei
• Energy rates due to weak decay rates of vanadium isotopes in stellar environment

Related

• Self-consistent microscopic calculations for electron captures on nuclei in core-collapse supernovae
• Electron Capture Rates of Mid-fp Shell Nuclei for Supernova and Stellar Evolution
• Sensitivity of stellar electron-capture rates to parent neutron number: A case study on a continuous chain of twenty Vanadium isotopes
• Stellar weak-interaction rates for rp-process waiting-point nuclei from projected shell model
• Stellar Weak Interaction Rates and Energy Losses for fp-Shell Nuclei Calculated in the Proton-Neutron Quasiparticle Random-Phase Approximation (II).(A = 61 to 80)