s过程中子源~（22）Ne +α的反应速率
Reaction rates for the s-process neutron source 22Ne+α
摘要：
22 Ne（α，n）25 Mg反应是s过程的重要中子源。在大质量恒星中，22 Ne（α，n）25 Mg是中子的主要来源，在核心氦燃烧和壳层碳燃烧时都是如此。在AGB星中，13 C（α，n）16 O反应是主要的中子源，而22 Ne +α反应主要影响热脉冲期间的s过程分支。竞争的22 Ne（α，n）25 Mg和22 Ne（α，γ）26 Mg反应的速率不确定性导致s过程核合成的大的变化。在这里，我们使用最近的实验结果和蒙特卡罗抽样来呈现最新且统计上严格的22 Ne +α反应速率。我们的新速率用于大质量恒星和AGB恒星的后处理核合成计算。我们表明，核合成的不确定性所产生的新的利率相比，以前发表的结果显着减少，但在目前的数据中的几个模糊性仍然必须加以解决。提出了进一步研究解决这些问题的建议。
英文摘要：
The 22Ne(α,n)25Mg reaction is an important source of neutrons for the s-process. In massive stars responsible for the weak component of the s-process, 22Ne(α,n)25Mg is the dominant source of neutrons, both during core helium burning and in shell carbon burning. For the main s-process component produced in Asymptotic Giant Branch (AGB) stars, the 13C(α,n)16O reaction is the dominant source of neutrons operating during the interpulse period, with the 22Ne+α source affecting mainly the s-process branchings during a thermal pulse. Rate uncertainties in the competing 22Ne(α,n)25Mg and 22Ne(α,γ)26Mg reactions result in large variations of s-process nucleosynthesis. Here, we present up-to-date and statistically rigorous 22Ne+α reaction rates using recent experimental results and Monte Carlo sampling. Our new rates are used in post-processing nucleosynthesis calculations both for massive stars and AGB stars. We demonstrate that the nucleosynthesis uncertainties arising from the new rates are dramatically reduced in comparison to previously published results, but several ambiguities in the present data must still be addressed. Recommendations for further study to resolve these issues are provided.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
