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Shell-model studies of the astrophysical rapid-proton-capture reaction P30(p,γ)S31

B. Alex Brown, W. A. Richter, and C. Wrede
Phys. Rev. C 89, 062801(R) – Published 30 June 2014; Erratum Phys. Rev. C 92, 069901 (2015)

Abstract

The thermonuclear rate of the reaction P30(p,γ)S31 is important for interpreting nova nucleosynthesis in the A30 region. Estimates based on shell-model calculations are complicated by high level density and the presence of negative-parity states in the resonance region near the proton-emission threshold. We present results for the first time of calculations in a full 1ω model space for the negative-parity states. Spectroscopic factors and proton-decay widths are calculated for input into the reaction rate. Available experimental data are used in conjunction with the calculations to obtain an estimate for the reaction rate. We show that the reaction rate will be uncertain to within about an order of magnitude until the position and decay widths of several of the key states in the region of 6.0 to 6.6 MeV are experimentally determined.

  • Figure
  • Received 23 February 2014
  • Revised 28 April 2014

DOI:https://doi.org/10.1103/PhysRevC.89.062801

©2014 American Physical Society

Erratum

Authors & Affiliations

B. Alex Brown1, W. A. Richter2,3, and C. Wrede1

  • 1Department of Physics and Astronomy and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824-1321, USA
  • 2iThemba LABS, P.O. Box 722, Somerset West 7129, South Africa
  • 3Department of Physics, University of the Western Cape, Private Bag X17, Bellville 7535, South Africa

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Issue

Vol. 89, Iss. 6 — June 2014

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