论文标题
重新评估$^{22} $ ne（$α，γ$）$^{26} $ mg和$^{22} $ ne（$α，n $）$^{25} $ mg反应费率
Re-evaluation of the $^{22}$Ne($α,γ$)$^{26}$Mg and $^{22}$Ne($α,n$)$^{25}$Mg reaction rates
论文作者
论文摘要
竞争$^{22} $ ne（$α，γ$）$^{26} $ mg和$^{22} $ ne（$α，n $）$^{25} $ mg反应控制着大型和AGB星星中弱$ s $ process的中子的产生。在这两个系统中，相应的反应速率之间的比率强烈影响总中子预算，并强烈影响最终的核合成。 $^{22} $ ne（$α，γ$）$^{26} $ mg和$^{22} $ ne（$α，n $）$^{25} $ mg反应率通过使用最近的各种实验性研究提供了$^{26} $ mg的新可用信息来重新评估。 Evaluations of The evaluated $^{22}$Ne($α,γ$)$^{26}$Mg reaction rate remains substantially similar to that of Longland {\it et al.} but, including recent results from Texas A\&M, the $^{22}$Ne($α,n$)$^{25}$Mg reaction rate is lower at a range of astrophysically important temperatures.使用牛顿和梅萨计算的恒星模型预测，由于$^{22} $ ne作为中子源的效率降低，弱分支$ s $过程的产生减少。使用MESA模型中的新反应速率导致$^{96} $ zr/$^{94} $ zr和$^{135} $ ba/$^{136} $ ba比率以更高的一致性与Presarlar Sic Crains的测得比率提高。
The competing $^{22}$Ne($α,γ$)$^{26}$Mg and $^{22}$Ne($α,n$)$^{25}$Mg reactions control the production of neutrons for the weak $s$-process in massive and AGB stars. In both systems, the ratio between the corresponding reaction rates strongly impacts the total neutron budget and strongly influences the final nucleosynthesis. The $^{22}$Ne($α,γ$)$^{26}$Mg and $^{22}$Ne($α,n$)$^{25}$Mg reaction rates was re-evaluated by using newly available information on $^{26}$Mg given by various recent experimental studies. Evaluations of The evaluated $^{22}$Ne($α,γ$)$^{26}$Mg reaction rate remains substantially similar to that of Longland {\it et al.} but, including recent results from Texas A\&M, the $^{22}$Ne($α,n$)$^{25}$Mg reaction rate is lower at a range of astrophysically important temperatures. Stellar models computed with NEWTON and MESA predict decreased production of the weak branch $s$-process due to the decreased efficiency of $^{22}$Ne as a neutron source. Using the new reaction rates in the MESA model results in $^{96}$Zr/$^{94}$Zr and $^{135}$Ba/$^{136}$Ba ratios in much better agreement with the measured ratios from presolar SiC grains.
