Abstract
Electron capture rates in Ni isotopes are studied in stellar environments, that is, at high densities and high temperatures during the core-collapse and postbounce explosive nucleosynthesis in supernovae. Reaction rates in $^{58}\mathrm{Ni}$ and $^{60}\mathrm{Ni}$, as well as in $^{56}\mathrm{Ni}$, $^{62}\mathrm{Ni}$, and $^{64}\mathrm{Ni}$, are evaluated by shell-model calculations with the use of a new shell-model Hamiltonian in the $\mathit{fp}$ shell, GXPF1J. While the previous shell-model calculations failed to reproduce the measured peaks of Gamow-Teller strength in $^{58}\mathrm{Ni}$ and $^{60}\mathrm{Ni}$, the present new Hamiltonian is found to reproduce them very well, as well as the capture rates obtained from the observed strengths. Strengths and energies of the Gamow-Teller transitions in $^{56}\mathrm{Ni}$, $^{62}\mathrm{Ni}$, and $^{64}\mathrm{Ni}$ are also found to be consistent with the observations.
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