Detailedβ-transition rates for URCA nuclear pairs in 8–10 solar-mass stars

Toki, Hiroshi; Suzuki, Toshio; Nomoto, Ken'ichi; Jones, Samuel; Hirschi, Raphael

Abstract

We calculate β-transition rates for URCA nuclear pairs using the sd-shell-model framework of Wildenthal [B. H. Widenthal, Prog. Part. Nucl. Phys. 11, 5 (1984)] with the modified Hamiltonian. We consider many β transitions including excited states necessary for electron capture and β decay with high Fermi energy of electrons at high electron density ρYe and temperature T relevant for the massive star and super-asymptotic-giant-branch star evolution. We provide β-transition rates for URCA nuclear pairs (A=23, 25, and 27) in the range of density 8.0 <log10ρYe< 9.2 in steps of 0.02 (Ye is the electron mole number and ρ is the nucleon density in units of g cm−3) and temperature 8.0 <log10T< 9.2 in steps of 0.05 (T is the temperature in units of K). This fine mesh is able to provide clearly the URCA density at log10ρYe=8.92 for A=23 and at log10ρYe=8.81 for A=25, while the URCA density is not clear for A=27. For the evolution of 8–10M⊙ stars, the use of the fine mesh is found to increase the cooling effect and affects the final fate of these stars.

Citation

Toki, H., Suzuki, T., Nomoto, K., Jones, S., & Hirschi, R. Detailedβ-transition rates for URCA nuclear pairs in 8–10 solar-mass stars. Physical Review C - Nuclear Physics, 88(1), Article 015806. https://doi.org/10.1103/physrevc.88.015806

• Journal Article Type: Article
• Online Publication Date: Jul 15, 2013
• Deposit Date: Jun 15, 2023
• Journal: Physical Review C
• Print ISSN: 0556-2813
• Electronic ISSN: 1089-490X
• Publisher: American Physical Society
• Peer Reviewed: Peer Reviewed
• Volume: 88
• Issue: 1
• Article Number: 015806
• DOI: https://doi.org/10.1103/physrevc.88.015806
• Keywords: Nuclear and High Energy Physics