AI 中文总结
本研究采用改进势团簇模型（MPCM）自洽计算14C相关反应，确定质子俘获超过中子俘获生成15N的转变温度，结果对天体物理核合成计算有重要意义。
AI 中文摘要
我们在同一改进势团簇模型（MPCM）内，开展了对相互竞争的14C(n,γ)15C与14C(p,γ)15N反应的首次自洽理论研究。针对14C(p,γ0)15N反应，利用受现有散射与束缚态数据约束的相互作用势，计算了总截面、天体物理S因子及反应率，估算得天体物理S因子S(0)=4.5(1) keV·b。结合我们近期对14C(n,γ)15C的MPCM计算结果，确定了在15N生成过程中质子俘获超过中子俘获的转变温度。在麦克斯韦-玻尔兹曼统计下，自洽比较预测转变温度T9^c.p.=2.5，显著高于此前的估算。分析扩展到 Tsallis 统计，表明偏离热平衡会使转变温度发生大幅偏移。这些结果为天体物理核合成计算提供了改进的核物理输入。
英文摘要
We present the first self-consistent theoretical study of the competing $^{14}\mathrm{C}(n,γ)^{15}\mathrm{C}$ and $^{14}\mathrm{C}(p,γ)^{15}\mathrm{N}$ reactions within the same modified potential cluster model (MPCM). For the $^{14}$C$(p,γ_{0})^{15}$N reaction, total cross sections, astrophysical $S$ factors, and reaction rates are calculated using interaction potentials constrained by the available scattering and bound-state data. The astrophysical $S$-factor is estimated as $S(0)=4.5(1)$~keV$\cdot \text{b}$. Combining these results with our recent MPCM calculations for $^{14}\mathrm{C}(n,γ)^{15}\mathrm{C}$, we determine the transition temperature at which proton capture overtakes neutron capture in the production of $^{15}\mathrm{N}$. The self-consistent comparison predicts a transition temperature $T_9^{\rm c.p.}=2.5$ under Maxwell--Boltzmann statistics, significantly higher than previous estimates. The analysis is extended to Tsallis statistics, demonstrating that deviations from thermal equilibrium produce substantial shifts of the transition temperature. These results provide improved nuclear-physics input for astrophysical nucleosynthesis calculations.
Comments7 pages, 5 figures
