恒星氦燃烧关键反应12C(&alpha;,&gamma;)16O天体物理S因子及其反应率

安振东; 马余刚; 范功涛; 陈振鹏

doi:10.11804/NuclPhysRev.34.03.437

恒星氦燃烧关键反应¹²C(α,γ)¹⁶O天体物理S因子及其反应率

doi: 10.11804/NuclPhysRev.34.03.437

1.
中山大学物理与天文学院, 广东珠海 519082;
2.
中国科学院上海应用物理研究所, 上海 201800;
3.
清华大学物理系, 北京 100084

基金项目: 国家自然科学基金面上项目（11175233，11220101005，91126017，11421505）；支持‘率先行动’中国博士后科学基金会与中国科学院联合资助优秀博士后项目（2016LH0045）；国家重点基础研究发展计划（973计划）（2014CB845401）

详细信息

作者简介:
安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

中图分类号: O571.42+2

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

1.
School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;
2.
Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;
3.
Department of Physics, Tsinghua University, Beijing 100084, China

Funds: National Natural Science Foundation of China (11175233, 11220101005, 91126017, 11421505); CPSF-CAS Joint Foundation for Excellent Postdoctoral Fellows (2016LH0045); National Basic Research Program of China (973 Program)(2014CB845401))

摘要: 恒星氦燃烧阶段3α反应和¹²C（α，γ）¹⁶O反应相互竞争，两者的反应率共同决定了氦燃烧结束后¹²C与¹⁶O的丰度比，该比值是大质量恒星后继演化以及伴随的元素核合成过程的初始条件。目前，氦燃烧¹²C（α，γ）¹⁶O反应起始T₉=0.2处，天体物理模型要求的反应率的精确度要低于10%，然而尚未有实验或理论给出满足要求的结果。最为直接和可靠地获取¹²C（α，γ）¹⁶O反应率的方法，就是尽可能往低能区测量其天体物理S因子，然后通过理论外推到感兴趣的能区。为此基于经典的R-矩阵理论，建立了适用于低能核反应的多道、多能级的约化R-矩阵理论来拟合几乎所有可用的¹⁶O系统的实验数据。配合使用协方差统计和误差传播理论，拟合外推得到了客观的、内部自恰的和唯一性好的¹²C（α，γ）¹⁶O反应天体物理S因子。总的外推S因子STOT（0.3 MeV）=162.7±7.3 keV·b，理论上首次给出达到恒星演化与元素核合成模型的最低要求的S因子。基于计算给出的全能区的S因子，数值积分给出了温度位于0.04 6 T₉ 6 10的¹²C（α，γ）¹⁶O天体物理反应率。在T₉=0.2处，推荐的反应率为（7.83 ±0.35）×10^-15 cm³mol^-1s^-1。

During stellar helium burning, the rates of 3α and the ¹²C(α,γ)¹⁶O reaction, in competition with one another, determine the relative abundances of ¹²C and ¹⁶O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of ¹²C(α,γ)¹⁶O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the ¹²C(α,γ)¹⁶O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of ¹²C(α,γ)¹⁶O, by a global fitting for almost all available experimental data of ¹⁶O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of ¹²C(α,γ)¹⁶O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of ¹²C(α,γ)¹⁶O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10^-15 cm³mol^-1s^-1, where stellar helium burning occurs.
- ¹²C (&alpha /
- ,&gamma /
- )¹⁶O反应 /
- S因子 /
- 天体热核反应率 /
- R-矩阵理论 /
- 恒星演化与元素核合成
Abstract: During stellar helium burning, the rates of 3α and the ¹²C(α,γ)¹⁶O reaction, in competition with one another, determine the relative abundances of ¹²C and ¹⁶O in a massive star. The abundance ratio is the beginning condition of the following nucleosynthesis and star evolution of massive stars, which are extremely sensitive to the rate of ¹²C(α,γ)¹⁶O reaction at T₉=0.2. The most direct and trustworthy way to obtain the reaction rate of the ¹²C(α,γ)¹⁶O reaction is to measure the S factor for that reaction to as low energy as possible, and to extrapolate to energies of astrophysical interest. Based on a new multilevel and multichannel reduced R-matrix theory for applications in nuclear astrophysics, we have obtained an accurate and self-consistent astrophysical S factor of ¹²C(α,γ)¹⁶O, by a global fitting for almost all available experimental data of ¹⁶O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of ¹²C(α,γ)¹⁶O was obtained with a recommended value STOT (0.3 MeV)=162.7±7.3 keV·b. And the reaction rates of ¹²C(α,γ)¹⁶O for stellar temperatures between 0.04 6 T₉ 6 10 are provided. At T₉=0.2, the reaction rate is (7.83 ±0.35)×10^-15 cm³mol^-1s^-1, where stellar helium burning occurs.
- ¹²C (&alpha /
- ,&gamma /
- )¹⁶O /
- S factor /
- thermonuclear reaction rate /
- R-matrix theory /
- nucleosynthesis and star evolution

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恒星氦燃烧关键反应¹²C(α,γ)¹⁶O天体物理S因子及其反应率

doi: 10.11804/NuclPhysRev.34.03.437

作者简介:
安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

计量

恒星氦燃烧关键反应¹²C(α,γ)¹⁶O天体物理S因子及其反应率

doi: 10.11804/NuclPhysRev.34.03.437

1. 中山大学物理与天文学院, 广东珠海 519082;

2. 中国科学院上海应用物理研究所, 上海 201800;

3. 清华大学物理系, 北京 100084

作者简介:
安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

English Abstract

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;

2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;

3. Department of Physics, Tsinghua University, Beijing 100084, China

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恒星氦燃烧关键反应12C(α,γ)16O天体物理S因子及其反应率

doi: 10.11804/NuclPhysRev.34.03.437

作者简介: 安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

Astrophysical S Factor and Reaction Rate of 12C(α,γ)16O Reaction in Stellar Helium Burning

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恒星氦燃烧关键反应12C(α,γ)16O天体物理S因子及其反应率

doi: 10.11804/NuclPhysRev.34.03.437

1. 中山大学物理与天文学院, 广东 珠海 519082; 2. 中国科学院上海应用物理研究所, 上海 201800; 3. 清华大学物理系, 北京 100084

作者简介: 安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

English Abstract

Astrophysical S Factor and Reaction Rate of 12C(α,γ)16O Reaction in Stellar Helium Burning

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China; 2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China; 3. Department of Physics, Tsinghua University, Beijing 100084, China

全文HTML

目录

恒星氦燃烧关键反应¹²C(α,γ)¹⁶O天体物理S因子及其反应率

作者简介:
安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

恒星氦燃烧关键反应¹²C(α,γ)¹⁶O天体物理S因子及其反应率

1. 中山大学物理与天文学院, 广东珠海 519082;

2. 中国科学院上海应用物理研究所, 上海 201800;

3. 清华大学物理系, 北京 100084

作者简介:
安振东(1985-),男,辽宁本溪人,副研究员,博士,从事核天体物理研究,E-mail:anzhendong@mail.sysu.edu.cn

Astrophysical S Factor and Reaction Rate of ¹²C(α,γ)¹⁶O Reaction in Stellar Helium Burning

1. School of Physics and Astronomy, Sun Yat-sen University, Zhuhai 519082, China;

2. Shanghai Institute of Applied Physics, Chinese Academy of Sciences, Shanghai 201800, China;

3. Department of Physics, Tsinghua University, Beijing 100084, China