Shell-model studies of the astrophysical rapid-proton-capture reaction 30P(p,γ)31S

被引：21
|
作者：
Brown, B. Alex [1 ,2 ]
Richter, W. A. [3 ,4 ]
Wrede, C. [1 ,2 ]
机构：
[1] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA
[2] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA
[3] iThemba LABS, ZA-7129 Somerset West, South Africa
[4] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa
来源：
PHYSICAL REVIEW C | 2014年 / 89卷 / 06期
基金：
美国国家科学基金会; 新加坡国家研究基金会;
关键词：
ENERGY-LEVELS; NOVA NUCLEOSYNTHESIS; NUCLEI;
D O I：
10.1103/PhysRevC.89.062801
中图分类号：
O57 [原子核物理学、高能物理学];
学科分类号：
070202 ;
摘要：
The thermonuclear rate of the reaction P-30(p,gamma)S-31 is important for interpreting nova nucleosynthesis in the A >= 30 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 1 (h) over bar omega. 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.
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页数：5
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