Shell-model calculations of stellar weak interaction rates. I. Gamow-Teller distributions and spectra of nuclei in the mass range A = 45–65

Abstract

Shell model calculations of stellar weak interaction rates: I. Gamow-Teller distributions and spectra of nuclei in the mass range A = 45 − 65 Electron capture and beta-decay rates on nuclei in the mass range A = 45 − 65 play an important role in many astrophysical environments. The determination of these rates by large-scale shell model calculations is desirable, but it requires to reproduce the Gamow-Teller strength distributions and spectra of the pf shell nuclei. We show in this paper that large-scale shell model calculations, employing a slightly monopole-corrected version of the wellknown KB3 interaction, fulfill these necessary requirements. In particular, our calculations reproduce the experimentally available GT+ and GT− strength distributions and the nuclear halflives, and describe the nuclear spectra appropriately.

Low-energy magnetic dipole response in 56Fe from high-resolution electron scattering

“…Efforts have been made to describe the corresponding strengths and their energy distributions in state-of-the-art shell-model calculations [13][14][15][16]. One finds that the stellar interaction rates must be considerably modified with respect to simplifying assumptions used so far in supernova models of massive stars [17].…”

Electron-capture Rates for pf-shell Nuclei in Stellar Environments and Nucleosynthesis

“…The B(GT − ) values for 56 Ni obtained with GXPF1J, KB3G and KBF [7] are shown in Fig. 1(a) together with the experimental data [8].…”

β -decay rate of Fe59 in shell burning environment and its influence on the production of Fe60Li1, Lam2, Qi3 et al. 2016Phys. Rev. C8070View full textAdd to dashboardCite

“…The LMP data set was based on a modified KB3 effective Hamiltonian developed from a realistic nucleon-nucleon interaction with optimization in the monopole interaction channel [9,10]. With more recent experimental data, the B(GT) resonances in the mass range 45≤A≤65 are better described globally for its application in the same temperature and density range than FFN.…”