{"title":"Radiative Capture of proton 14N(p,γ)15O at Low Energy","authors":"B. Irgaziev, A. Kabir, J. Nabi","doi":"10.1088/1674-1137/ad1b3c","DOIUrl":null,"url":null,"abstract":"\n The CNO cycle is the main source of energy in stars more massive than our Sun. It defines the energy production and the duration contributes in determining the lifetime of massive stars. The cycle is an important tool for the determination of the age of globular clusters. Radiative capture p + 14N →15O + γ, at energies of astrophysical interest, is one of the important processes in the CNO cycle. In this project, we apply a potential model to describe both non-resonant and resonant reactions in the channels where radiative capture occurs through electric E1 transitions. We employed the R-matrix method to describe the reactions going via M1 resonant transitions, when it was not possible to correctly reproduce the experimental data by a potential model. The partial components of the astrophysical S-factor were calculated for all possible electric and magnetic dipole transitions in 15O. The linear extrapolated S-factor at zero energy (S(0)) is in good agreement with earlier reported values for all types of transitions considered in this work. Based on the value of the total astrophysical S-factor, depending on the collision energy, we calculate the nuclear reaction rates for p + 14N →15O + γ. The computed rates are in good agreement with the results of the NACRE II Collaboration.","PeriodicalId":504778,"journal":{"name":"Chinese Physics C","volume":"8 2","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-01-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Chinese Physics C","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1088/1674-1137/ad1b3c","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
Abstract
The CNO cycle is the main source of energy in stars more massive than our Sun. It defines the energy production and the duration contributes in determining the lifetime of massive stars. The cycle is an important tool for the determination of the age of globular clusters. Radiative capture p + 14N →15O + γ, at energies of astrophysical interest, is one of the important processes in the CNO cycle. In this project, we apply a potential model to describe both non-resonant and resonant reactions in the channels where radiative capture occurs through electric E1 transitions. We employed the R-matrix method to describe the reactions going via M1 resonant transitions, when it was not possible to correctly reproduce the experimental data by a potential model. The partial components of the astrophysical S-factor were calculated for all possible electric and magnetic dipole transitions in 15O. The linear extrapolated S-factor at zero energy (S(0)) is in good agreement with earlier reported values for all types of transitions considered in this work. Based on the value of the total astrophysical S-factor, depending on the collision energy, we calculate the nuclear reaction rates for p + 14N →15O + γ. The computed rates are in good agreement with the results of the NACRE II Collaboration.
一氧化碳循环是比太阳质量更大的恒星的主要能量来源。它决定了能量的产生和持续时间,有助于确定大质量恒星的寿命。该周期是确定球状星团年龄的重要工具。在具有天体物理学意义的能量下,辐射捕获 p + 14N →15O + γ 是 CNO 循环的重要过程之一。在本项目中,我们采用了一种势能模型来描述通过电 E1 变换发生辐射俘获的通道中的非共振和共振反应。当电势模型无法正确再现实验数据时,我们采用了 R 矩阵方法来描述通过 M1 共振跃迁发生的反应。我们计算了 15O 中所有可能的电偶极和磁偶极跃迁的天体物理 S 因子的部分分量。零能量(S(0))时的线性外推 S 因子与之前报道的本研究中所有类型跃迁的 S 因子值非常吻合。根据天体物理 S 因子的总值(取决于碰撞能量),我们计算了 p + 14N →15O + γ 的核反应速率。 计算出的速率与 NACRE II 合作组的结果非常一致。