Abstract
Electron-capture (e-capture) and β-decay rates in sd-shell are evaluated by shell-model calculations with the USDB Hamiltonian in stellar environments with fine grids of density and temperature. The weak rates are used to study the evolution of ONeMg cores in stars with 8–10 M⊙. Important roles of the nuclear Urca processes for the nuclear pairs with A = 23 and 25 on the cooling of the cores are investigated. The rates are also used to study heating of the cores by double e-capture processes on 24Mg and 20Ne in later stages of the evolution. In particular, the e-capture rates for a second-forbidden transition in 20Ne are evaluated with the multipole expansion method of Walecka as well as the method of Behrens-B\(\ddot {\mbox{u}}\)hring. Possible important contributions of the transition to heating the ONeMg core and implications on the final fate of the core are discussed, whether it ends with core-collapse e-capture supernova (ECSN) or thermonuclear expansion.
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Acknowledgements
The author would like to thank K. Nomoto, S. Zha, S.-C. Leung, and H. Toki for the collaboration of the present work. This work was supported in part by JSPS KAKENHI grant No. JP19K03855. He also thanks NAOJ Japan for accepting him as a visiting researcher during the period of the work.
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Suzuki, T. (2023). Weak Interactions in Evolving Stars. In: Tanihata, I., Toki, H., Kajino, T. (eds) Handbook of Nuclear Physics . Springer, Singapore. https://doi.org/10.1007/978-981-15-8818-1_117-1
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