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.

引用

页数：10

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