Thermonuclear 19F(p, α)16O Reaction Rate Revised and Astrophysical Implications

被引:4
|
作者
Zhang, L. Y. [1 ,2 ]
Lopez, A. Y. [3 ]
Lugaro, M. [3 ,4 ,5 ]
He, J. J. [1 ,2 ]
Karakas, A. I. [5 ,6 ]
机构
[1] Beijing Normal Univ, Coll Nucl Sci & Technol, Key Lab Beam Technol, Minist Educ, Beijing 100875, Peoples R China
[2] Beijing Radiat Ctr, Beijing 100875, Peoples R China
[3] Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
[4] Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary
[5] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia
[6] ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Stromlo, Australia
来源
ASTROPHYSICAL JOURNAL | 2021年 / 913卷 / 01期
基金
澳大利亚研究理事会; 中国国家自然科学基金;
关键词
ASYMPTOTIC GIANT BRANCH; RESONANCE STRENGTHS; CROSS-SECTION; ENERGY-LEVELS; LIGHT-NUCLEI; FLUORINE; STARS; F-19(P; ALPHA-GAMMA)O-16; NUCLEOSYNTHESIS; CARBON;
D O I
10.3847/1538-4357/abef63
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have calculated the thermonuclear F-19(p, alpha ( gamma ))O-16 reaction rate in a wide temperature region of 0.001-10 GK by re-evaluating the available experimental data. Together with recently evaluated (19)(p, alpha (0))O-16 and (19)(p, alpha ( pi ))O-16 data, we have derived a new total reaction rate of F-19(p, alpha)O-16 using a Monte Carlo technique. The present rate is larger than the NACRE recommended one by factors of 36.4, 2.3, and 1.7 at temperatures of 0.01, 0.05, and 0.1 GK, respectively. This is because we have considered the enhanced low-energy astrophysical S factors in the (p, alpha ( gamma )) channel, owing to the interference effect between an 11 keV resonance and the well-known 323 keV resonance. It shows that the (p, alpha ( gamma )) channel dominates the total rate over the entire temperature region, except for a narrow region of 0.05-0.12 GK where the (p, alpha (0)) channel dominates, contrary to the previous conclusion. We have investigated the impact of the F-19(p, alpha)O-16 reaction rate using a simple parametric model of extra mixing in low-mass AGB stars, which would lower the fluorine abundance produced and observed in these stars. However, models considering different temperature profiles and more sophisticated approaches, such as extra mixing induced by magnetic fields, are needed to verify the results of our preliminary tests. Interestingly, our new rate has a strong impact on destruction of F-19 in the CNO cycle at low temperatures of 0.02-0.03 GK, and this general behavior needs to be analyzed further.
引用
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页数:13
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