13N(d,n)14O reaction and the astrophysical 13N(p,γ)14O reaction rate

被引：32

作者：

Li, Z. H. ^{[1
]}

Guo, B. ^{[1
]}

Yan, S. Q. ^{[1
]}

Lian, G. ^{[1
]}

Bai, X. X. ^{[1
]}

Wang, Y. B. ^{[1
]}

Zeng, S. ^{[1
]}

Su, J. ^{[1
]}

Wang, B. X. ^{[1
]}

Liu, W. P. ^{[1
]}

Shu, N. C. ^{[1
]}

Chen, Y. S. ^{[1
]}

Chang, H. W. ^{[1
]}

Jiang, L. Y. ^{[1
]}

机构：

[1] Inst Atom Energy, Beijing 102413, Peoples R China

来源：

PHYSICAL REVIEW C | 2006年 / 74卷 / 03期

关键词：

D O I：

10.1103/PhysRevC.74.035801

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：

N-13(p,gamma)O-14 is one of the key reactions in the hot CNO cycle which occurs at stellar temperatures around T-9 >= 0.1. Up to now, some uncertainties still exist for the direct capture component in this reaction, thus an independent measurement is of importance. In present work, the angular distribution of the N-13(d,n)O-14 reaction at E-c.m.=8.9 MeV has been measured in inverse kinematics, for the first time. Based on the distorted-wave Born approximation (DWBA) analysis, the nuclear asymptotic normalization coefficient (ANC), (C1,1/2O)-O-14, for the ground state of O-14 -> N-13 + p is derived to be 5.42 +/- 0.48 fm(-1/2). The N-13(p,gamma)O-14 reaction is analyzed with the R-matrix approach, its astrophysical S factors and reaction rates at energies of astrophysical relevance are then determined with the ANC. The implications of the present reaction rates on the evolution of novae are then discussed with the reaction network calculations.

引用

页数：7

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