The ${}^{22}\mathrm{Ne}(p,\gamma ){}^{23}\mathrm{Na}$ capture reaction is a key step in the Ne-Na cycle of hydrogen burning. The rate of this reaction is critical in classical novae nucleosynthesis and hot bottom burning (HBB) processes in asymptotic giant branch (AGB) stars. Despite its astrophysical importance, significant uncertainty remains in the reaction rate due to several narrow low-energy resonances lying within and near the Gamow window. The present work revisits this reaction by examining the contribution of the 8664 keV subthreshold state and the 8945 keV doublet resonance state of $7/2^{-}$ configuration in ${}^{23}\mathrm{Na}$. Finite range distorted-wave Born approximation (FRDWBA) analysis of existing ${}^{22}\mathrm{Ne}({}^3\mathrm{He},d){}^{23}\mathrm{Na}$ transfer reaction data was carried out to extract the peripheral asymptotic normalization coefficients (ANCs) of the 8664 keV state. The ANC value obtained in the present work is $\approx 25\%$ higher compared to the previous work by Santra et al. [Phys. Rev. C 101, 025802 (2020)]. Systematic $R$-matrix calculations were performed to obtain the nonresonant astrophysical $S$ factor utilizing the enhanced ANC value. The resonance strengths of the 8945 keV doublets were deduced from shell model calculations. The rate calculations are performed by omitting the resonances at $E_x=8862$, 8894, and 9000 keV, which are unlikely to exist as reported by Carrasco-Rojas et al. [Phys. Rev. C 108, 045802 (2023)]. The total reaction rate is found to be $\approx 15–20\%$ higher at temperatures relevant for the HBB processes, compared to the recent rate measured by Williams et al. [Phys. Rev. C 102, 035801 (2020)], and matches their rate at temperatures of interest for classical novae nucleosynthesis.

中文翻译：

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Ne22(p,γ)Na23反应速率的重新评估

这${}^{22}氖（p,\gamma ）{}^{23}钠$捕获反应是氢燃烧Ne-Na循环中的关键步骤。这种反应的速率对于渐近巨分支（AGB）恒星的经典新星核合成和热底燃烧（HBB）过程至关重要。尽管其天体物理重要性，但由于伽莫夫窗内和附近的几个狭窄的低能共振，反应速率仍然存在很大的不确定性。目前的工作通过检查 8664 keV 亚阈值状态和 8945 keV 双峰共振态的贡献来重新审视该反应。$7/2^{-}$配置在${}^{23}钠$。现有有限范围畸变波玻恩近似 (FR​​DWBA) 分析${}^{22}氖（{}^3他,d）{}^{23}钠$进行转移反应数据以提取8664 keV态的外周渐近归一化系数（ANC）。本工作中获得的 ANC 值为$\approx 25\%$与 Santra等人之前的工作相比更高。 [物理。修订版 C 101 , 025802 (2020)]。系统化$右$-进行矩阵计算以获得非共振天体物理$S$利用增强的 ANC 值的因素。 8945 keV 双峰的共振强度是通过壳模型计算得出的。速率计算是通过忽略共振来进行的${乙}_X=8862$、8894 和 9000 keV，如 Carrasco-Rojas等人报道的那样不太可能存在。 [物理。修订版 C 108 , 045802 (2023)]。发现总反应速率为$\approx 15–20\%$与 Williams等人最近测量的速率相比，与 HBB 过程相关的温度更高。 [物理。 Rev. C 102 , 035801 (2020)]，并与经典新星核合成感兴趣的温度下的速率相匹配。