恒星氦燃烧关键反应^(12)C(α,γ)^(16)O天体物理S因子及其反应率  

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

作　　者：安振东 马余刚[2] 范功涛[2] 陈振鹏[3] 

机构地区：[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

出　　处：《原子核物理评论》2017年第3期437-445,共9页Nuclear Physics Review

基　　金：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)~~

摘　　要：恒星氦燃烧阶段3α反应和^(12)C(α,γ)^(16)O反应相互竞争,两者的反应率共同决定了氦燃烧结束后^(12)C与^(16)O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^(12)C(α,γ)^(16)O反应起始T_9=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^(12)C(α,γ)^(16)O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^(16)O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^(12)C(α,γ)^(16)O反应天体物理S因子。总的外推S因子STOT(0.3 Me V)=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≤T_9≤10的^(12)C(α,γ)^(16)O天体物理反应率。在T_9=0.2处,推荐的反应率为(7.83±0.35)×10^(-15)cm^3mol^(-1)s^(-1)。During stellar helium burning, the rates of 3α and the12^C（α,γ）16^O reaction, in competition with one another, determine the relative abundances of12^C and16^O 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 of12^C（α,γ）16^O reaction at T9 = 0.2. The most direct and trustworthy way to obtain the reaction rate of the12^C（α,γ）16^O 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 of12^C（α,γ）16^O, by a global fitting for almost all available experimental data of16^O system, with the coordination of covariance statistics and error-propagation theory. The extrapolated S factor of12^C（α,γ）16^O was obtained with a recommended value STOT（0.3 Me V） = 162.7±7.3 keV·b. And the reaction rates of^（12）C（α, γ）^（16）O for stellar temperatures between 0.04≤T9≤10 are provided. At T9 = 0.2, the reaction rate is（7.83 ± 0.35）×10^-15 cm^3 mol^-1 s^-1, where stellar helium burning occurs.

关 键 词：12^C(α γ)16^O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 

分 类 号：O571.422[理学—粒子物理与原子核物理]