Shell-model studies of the astrophysical rp reaction 29P(p,γ)30S

被引：9
|
作者：
Richter, W. A. [1 ,2 ]
Brown, B. Alex [3 ,4 ]
机构：
[1] iThemba LABS, ZA-7129 Somerset West, South Africa
[2] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa
[3] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA
[4] Michigan State Univ, Natl Superconducting Cyclotron Lab, E Lansing, MI 48824 USA
来源：
PHYSICAL REVIEW C | 2013年 / 87卷 / 06期
基金：
新加坡国家研究基金会; 美国国家科学基金会;
关键词：
THERMONUCLEAR REACTION-RATES;
D O I：
10.1103/PhysRevC.87.065803
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：
We present results for levels in S-30 (the mirror nucleus of Si-30) that are used for the P-29(p,gamma) rp reaction rate calculations. The resonance energies used in the reaction rate calculations are based on recent measurements which extend the excitation energy spectrum. The levels are checked against results from the isobaric mass multiplet equation and the binding energies of the T = 1 analog states. Where the analog states are not known the levels are calculated with two-body interactions that use the sd-shell interactions USDA and USDB as the charge-independent parts, with a Coulomb, charge-dependent, and charge-asymmetric Hamiltonian added. The gamma-decay lifetimes and P-29 to S-30 spectroscopic factors are also calculated with the same interactions, and together with experimental information on the levels of excited states are used to determine the P-29(p,gamma)S-30 reaction rates.
引用
收藏
页数：7
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