Measurement of the Gamow-Teller strength distribution in Co58 via the Ni58(t,He3) reaction at 115 MeV/nucleon

A. L. Cole, H. Akimune, Sam M. Austin, D. Bazin, A. M. van den Berg, G. P. A. Berg, J. Brown, I. Daito, Y. Fujita, M. Fujiwara, S. Gupta, K. Hara, M. N. Harakeh, J. Jänecke, T. Kawabata, T. Nakamura, D. A. Roberts, B. M. Sherrill, M. Steiner, H. Ueno, and R. G. T. Zegers
Phys. Rev. C 74, 034333 – Published 29 September 2006

Abstract

Electron capture and β decay play important roles in the evolution of presupernovae stars and their eventual core collapse. These rates are normally predicted through shell-model calculations. Experimentally determined strength distributions from charge-exchange reactions are needed to test modern shell-model calculations. We report on the measurement of the Gamow-Teller strength distribution in Co58 from the Ni58(t,He3) reaction with a secondary triton beam of an intensity of ~106 pps at 115 MeV/nucleon and a resolution of ~250 keV. Previous measurements with the Ni58(n,p) and the Ni58(d,He2) reactions were inconsistent with each other. Our results support the latter. We also compare the results to predictions of large-scale shell-model calculations using the KB3G and GXPF1 interactions and investigate the impact of differences between the various experiments and theories in terms of the weak rates in the stellar environment. Finally, the systematic uncertainties in the normalization of the strength distribution extracted from Ni58(He3, t) are described and turn out to be nonnegligible due to large interferences between the ΔL=0,ΔS=1 Gamow-Teller amplitude and the ΔL=2,ΔS=1 amplitude.

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  • Received 20 March 2006

DOI:https://doi.org/10.1103/PhysRevC.74.034333

©2006 American Physical Society

Authors & Affiliations

A. L. Cole1,2,*, H. Akimune3, Sam M. Austin1,2,4, D. Bazin1, A. M. van den Berg5, G. P. A. Berg6,7, J. Brown8, I. Daito9, Y. Fujita10, M. Fujiwara9,11, S. Gupta1,2, K. Hara11, M. N. Harakeh12, J. Jänecke13, T. Kawabata14, T. Nakamura15, D. A. Roberts13, B. M. Sherrill1,2,4, M. Steiner1, H. Ueno16, and R. G. T. Zegers1,2,4,†

  • 1National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824-1321, USA
  • 2Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
  • 3Department of Physics, Konan University, 8-9-1 Okamoto Higashinda, Kobe, Hyogo, 658-8501, Japan
  • 4Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
  • 5Kernfysisch Versneller Instituut, University of Groningen, Zernikelaan 25, 9747 AA Groningen, The Netherlands
  • 6Department of Physics, University of Notre Dame, Indiana 46556-5670, USA
  • 7Joint Institute for Nuclear Astrophysics, University of Notre Dame, Indiana 46556-5670, USA
  • 8Department of Physics, Wabash College, Crawfordsville, Indiana 47933, USA
  • 9Kansai Photon Science Institute, Japan Atomic Research Institute, Kizu Kyoto 619-0215, Japan
  • 10Department of Physics, Osaka University, Toyonaka, Osaka 560-0043, Japan
  • 11Research Center for Nuclear Physics, Osaka University, Ibaraki, Osaka 567-0047, Japan
  • 12Kernfysisch Versneller Instituut, Zernikelaan 25 9747 AA Groningen, The Netherlands
  • 13Department of Physics, University of Michigan, Ann Arbor, Michigan 48109-1040, USA
  • 14Center for Nuclear Study, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
  • 15Tokyo Institute of Technology, 2-12-1 O-Okayama, Tokyo 152-8550, Japan
  • 16Applied Nuclear Physics Laboratory, RIKEN, Wako, Saitama 351-0198, Japan

  • *Present address: Department of Physics, University of Michigan, Ann Arbor, Michigan 48109-1040, USA.
  • Electronic address: zegers@nscl.msu.edu

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Vol. 74, Iss. 3 — September 2006

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