Electron Capture Reactions and Beta Decays in Steller Environments

Journal Article · Fri Oct 28 00:00:00 EDT 2011 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3628352· OSTI ID:21612067

Suzuki, T ^[1]; Mao, H ^[2]; Honma, M ^[3]; Yoshida, T ^[4]; Kajino, T ^[5]; Otsuka, T ^[6]

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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 and Center for Nuclear Study, University of Tokyo, Hirosawa, Wako-shi, Saitama, 351-0198 (Japan)
2. Graduate School of Integrated Basic Sciences, Nihon University, Sakurajosui-3-25-40, Setagaya-ku, Tokyo 156-8550, Japan and ENSPS, Pole API-Parc d'Innovation, Boulevard Sebastien Brant, BP 10413, 67412 ILLKIRCH CEDEXL (France)
3. Center for Mathematical Sciences, University of Aizu, Aizu-Wakamatsu, Fukushima 965-8580 (Japan)
4. Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)
5. Department of Astronomy, Graduate School of Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan) and National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan)
6. Department of Physics and Center for Nuclear Study, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan) and RIKEN, Hirosawa, Wako-shi, Saitama 351-0198 (Japan)

Electron capture reactions on Ni and Co isotopes are investigated by shell model calculations in steller environments. The capture rates depend sensitively on the distribution of the Gamow-Teller (GT) strength. The capture rates obtained by using GXPF1J Hamiltonian for fp-shell are found to be consistent with the rates obtained from experimental GT strength in {sup 58}Ni and {sup 60}Ni. Capture rates in Co isotopes, where there were large discrepancies among previous calculations, are also investigated. Beta decays of the N = 126 isotones are studied by shell model calculations taking into account both the GT and first-forbidden (FF) transitions. The FF transitions are found to be important to reduce the half-lives by twice to several times of those by the GT contributions only. Implications of the short half-lives of the waiting point nuclei on the r-process nucleosynthesis are discussed for various astrophysical conditions.

• OSTI ID: 21612067
• Journal Information: AIP Conference Proceedings, Vol. 1377, Issue 1; Conference: FINUSTAR 3 Conference on frontiers in nuclear structure, astrophysics, and reactions, Rhodes (Greece), 23-27 Aug 2010; Other Information: DOI: 10.1063/1.3628352; (c) 2011 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
ASTROPHYSICS
BARYONS
BETA DECAY
COBALT ISOTOPES
ELECTRON CAPTURE
GAMOW-TELLER RULES
HALF-LIFE
HAMILTONIANS
ISOTONIC NUCLEI
NICKEL 58
NICKEL 60
NUCLEAR STRUCTURE
NUCLEOSYNTHESIS
R PROCESS
SHELL MODELS
CAPTURE
DECAY
ELEMENTARY PARTICLES
EVEN-EVEN NUCLEI
EVOLUTION
FERMIONS
HADRONS
INTERMEDIATE MASS NUCLEI
ISOTOPES
MATHEMATICAL MODELS
MATHEMATICAL OPERATORS
NICKEL ISOTOPES
NUCLEAR DECAY
NUCLEAR MODELS
NUCLEI
PHYSICS
QUANTUM OPERATORS
STABLE ISOTOPES
STAR EVOLUTION
SYNTHESIS