Stellar electron-capture rates calculated with the finite-temperature relativistic random-phase approximation

被引：71
|
作者：
Niu, Y. F. [1 ]
Paar, N. [2 ]
Vretenar, D. [2 ]
Meng, J. [1 ,3 ,4 ]
机构：
[1] Peking Univ, Sch Phys, State Key Lab Nucl Phys & Technol, Beijing 100871, Peoples R China
[2] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 41000, Croatia
[3] Beihang Univ, Sch Phys & Nucl Energy Engn, Beijing 100191, Peoples R China
[4] Univ Stellenbosch, Dept Phys, ZA-7602 Stellenbosch, South Africa
来源：
PHYSICAL REVIEW C | 2011年 / 83卷 / 04期
关键词：
WEAK-INTERACTION RATES; INTERMEDIATE-MASS NUCLEI; HARTREE-BOGOLIUBOV THEORY; SHELL-MODEL CALCULATIONS; MEAN-FIELD THEORY; RATE TABLES; FP-SHELL; DISTRIBUTIONS; SUPERNOVAE; COLLAPSE;
D O I：
10.1103/PhysRevC.83.045807
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 introduce a self-consistent microscopic theoretical framework for modeling the process of electron capture on nuclei in stellar environment, based on relativistic energy density functionals. The finite-temperature relativistic mean-field model is used to calculate the single-nucleon basis and the occupation factors in a target nucleus, and J(pi) = 0(+/-), 1(+/-), and 2(+/-) charge-exchange transitions are described by the self-consistent finite-temperature relativistic random-phase approximation. Cross sections and rates are calculated for electron capture on Fe-54,Fe-56 and Ge-76,Ge-78 in stellar environment, and results compared with predictions of similar and complementary model calculations.
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页数：10
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