Astrophysical reaction rates from statistical model calculations
Astrophysical reaction rates from statistical model calculations
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DOI：
10.1006/adnd.2000.0834
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发表时间：
2000-05-01
影响因子：
1.8
通讯作者：
Thielemann, FK
中科院分区：
文献类型：
--
作者：
Rauscher, T;Thielemann, FK
对于10小于等于Z小于等于83（Ne到Bi）的靶和达到中子和质子滴线的质量范围，在统计模型（Hauser-Feshbach形式主义）中计算了温度范围为0.01 x 10（9）小于等于T（K）小于等于10.0 x 10（9）的理论反应速率。所考虑的反应是（n，gamma）、（n，p）、（n，alpha）、（p，gamma）、（p，alpha）、（alpha，gamma）及其逆反应。反应速率作为热填充目标的温度的函数给出了七个分析参数拟合。为了便于与实验速率进行比较，还列出了恒星增强因子。计算了两套完整的速率，其中之一包括对丰中子核壳层猝灭的唯象处理。这些广泛的数据集以电子文件的形式在线提供，而从一项计算中选出的子集则以印刷表格的形式提供。包括理论输入和使用所提供表格的建议的摘要。(C)北京大学出版社.
Theoretical reaction rates in the temperature range 0.01 x 10(9) less than or equal to T(K) less than or equal to 10.0 x 10(9) are calculated in the statistical model (Hauser-Feshbach formalism) for targets with 10 less than or equal to Z less than or equal to 83 (Ne to Bi) and for a mass range reaching the neutron and proton driplines. Reactions considered are (n, gamma), (n, p), (n, alpha), (p, gamma), (p, alpha), (alpha, gamma), and their inverse reactions. Reaction rates as a function of temperature for thermally populated targets are given by seven analytical parameter fits. To facilitate comparison with experimental rates, the stellar enhancement factors are also tabulated. Two complete sets of rates have been calculated, one of which includes a phenomenological treatment of shell quenching for neutron-rich nuclei. These extensive datasets are provided on-line as electronic files, while a selected subset from one calculation is given as printed tables. A summary of the theoretical inputs and advice on the use of the provided tabulations is included. (C) 2000 Academic Press.