Stellar electron-capture rates calculated with the finite-temperature relativistic random-phase approximation

Abstract

We introduce a self-consistent microscopic theoretical framework for modelling the process of electron capture on nuclei in stellar environment, based on relativistic energy density functionals. The finite-temperature relativistic mean-field model is used to calculate the single-nucleon basis and the occupation factors in a target nucleus, and $J^{\pi }=0^{\pm }$, $1^{\pm }$, $2^{\pm }$ charge-exchange transitions are described by the self-consistent finite-temperature relativistic random-phase approximation. Cross sections and rates are calculated for electron capture on 54,56Fe and 76,78Ge in stellar environment, and results compared with predictions of similar and complementary model calculations.

Physical Review C, accepted

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• Theory of Core-Collapse Supernovae
• Exotic modes of excitation in atomic nuclei far from stability
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Cited by in corpus (10)

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• Gamow-Teller response and its spreading mechanism in doubly magic nuclei
• Quasi-particle random phase approximation with quasi-particle-vibration coupling: application to the Gamow-Teller response of the superfluid nucleus ${}^{120}$Sn
• Nucleon self-energies for supernova equations of state
• Unblocking of stellar electron capture for neutron-rich $N=50$ nuclei at finite temperature
• Stellar electron capture rates on neutron-rich nuclei and their impact on core-collapse
• Impact of complex many-body correlations on electron capture in thermally excited nuclei around ${}^{78}$Ni
• Finite-temperature electron-capture rates for neutron-rich nuclei around N=50 and effects on core-collapse supernovae simulations
• Role of quadrupole deformation and continuum effects in the "island of inversion'' nuclei ${}^{28,29,31}$F
• Sensitivity of $\beta$-decay rates to the radial dependence of the nucleon effective mass