NEW DETERMINATION OF THE 13C(α, n)16O REACTION RATE AND ITS INFLUENCE ON THE s-PROCESS NUCLEOSYNTHESIS IN AGB STARS

被引：64

作者：

Guo, B. ^{[1
]}

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

Lugaro, M. ^{[2
]}

Buntain, J. ^{[2
]}

Pang, D. Y. ^{[3
,4
]}

Li, Y. J. ^{[1
]}

Su, J. ^{[1
]}

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

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

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

Fan, Q. W. ^{[1
]}

Jin, S. J. ^{[1
]}

Karakas, A. I. ^{[5
]}

Li, E. T. ^{[1
]}

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

Lian, G. ^{[1
]}

Liu, J. C. ^{[1
]}

Liu, X. ^{[1
]}

Shi, J. R. ^{[6
]}

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

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

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

Zeng, S. ^{[1
]}

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

机构：

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

[2] Monash Univ, Monash Ctr Astrophys, Clayton, Vic 3800, Australia

[3] Peking Univ, State Key Lab Nucl Phys & Technol, Beijing 100871, Peoples R China

[4] Peking Univ, Sch Phys, Beijing 100871, Peoples R China

[5] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[6] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 756卷 / 02期

基金：

中国国家自然科学基金;

关键词：

nuclear reactions; nucleosynthesis; abundances; stars: AGB and post-AGB; ASYMPTOTIC-GIANT-BRANCH; LOW-MASS; NEUTRON-CAPTURE; EVOLUTION; MODELS; ZIRCONIUM; GRAINS; YIELDS;

D O I：

10.1088/0004-637X/756/2/193

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a new measurement of the alpha-spectroscopic factor (S-alpha) and the asymptotic normalization coefficient for the 6.356 MeV 1/2(+) subthreshold state of O-17 through the C-13(B-11, Li-7)O-17 transfer reaction and we determine the alpha-width of this state. This is believed to have a strong effect on the rate of the C-13(alpha, n)O-16 reaction, the main neutron source for slow neutron captures (the s-process) in asymptotic giant branch (AGB) stars. Based on the new width we derive the astrophysical S-factor and the stellar rate of the C-13(alpha, n)O-16 reaction. At a temperature of 100 MK, our rate is roughly two times larger than that by Caughlan & Fowler and two times smaller than that recommended by the NACRE compilation. We use the new rate and different rates available in the literature as input in simulations of AGB stars to study their influence on the abundances of selected s-process elements and isotopic ratios. There are no changes in the final results using the different rates for the C-13(alpha, n)O-16 reaction when the C-13 burns completely in radiative conditions. When the C-13 burns in convective conditions, as in stars of initial mass lower than similar to 2 M-circle dot and in post-AGB stars, some changes are to be expected, e.g., of up to 25% for Pb in our models. These variations will have to be carefully analyzed when more accurate stellar mixing models and more precise observational constraints are available.

引用

页数：10

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