Evaluation of electron capture reaction rates in Ni isotopes in stellar environments

Journal Article · Fri Apr 15 00:00:00 EDT 2011 · Physical Review. C, Nuclear Physics

DOI:https://doi.org/10.1103/PHYSREVC.83.044619· OSTI ID:21499598

Suzuki, Toshio ^[1]; Honma, Michio ^[2]; Mao, Helene ^[3]; Otsuka, Takaharu ^[4]; Kajino, Toshitaka ^[5]

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1. Department of Physics and Graduate School of Integrated Basic Sciences, College of Humanities and Sciences, Nihon University Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550 (Japan)
2. Center for Mathematical Sciences, University of Aizu, Aizu-Wakamatsu, Fukushima 965-8580 (Japan)
3. ENSPS, Pole API-Parc d'Innovation, Boulevard Sebastien Brant, BP 10413, F-67412 Illkirch Cedex (France)
4. Department of Physics and Center for Nuclear Study, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)
5. National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan)

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 {sup 58}Ni and {sup 60}Ni, as well as in {sup 56}Ni, {sup 62}Ni, and {sup 64}Ni, are evaluated by shell-model calculations with the use of a new shell-model Hamiltonian in the fp shell, GXPF1J. While the previous shell-model calculations failed to reproduce the measured peaks of Gamow-Teller strength in {sup 58}Ni and {sup 60}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 {sup 56}Ni, {sup 62}Ni, and {sup 64}Ni are also found to be consistent with the observations.

• OSTI ID: 21499598
• Journal Information: Physical Review. C, Nuclear Physics, Vol. 83, Issue 4; Other Information: DOI: 10.1103/PhysRevC.83.044619; (c) 2011 American Institute of Physics; ISSN 0556-2813
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
COMPUTERIZED SIMULATION
ELECTRON CAPTURE
EVALUATION
EXPLOSIVES
GAMOW-TELLER RULES
HAMILTONIANS
NICKEL 56
NICKEL 58
NICKEL 60
NICKEL 62
NICKEL 64
NUCLEOSYNTHESIS
REACTION KINETICS
SHELL MODELS
STARS
SUPERNOVAE
BETA DECAY RADIOISOTOPES
BETA-PLUS DECAY RADIOISOTOPES
BINARY STARS
CAPTURE
DAYS LIVING RADIOISOTOPES
ELECTRON CAPTURE RADIOISOTOPES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
INTERMEDIATE MASS NUCLEI
ISOTOPES
KINETICS
MATHEMATICAL MODELS
MATHEMATICAL OPERATORS
NICKEL ISOTOPES
NUCLEAR MODELS
NUCLEI
QUANTUM OPERATORS
RADIOISOTOPES
SIMULATION
STABLE ISOTOPES
SYNTHESIS
VARIABLE STARS