In stellar hydrogen burning, the carbon-nitrogen-oxygen (CNO) cycle dominates, with the ${}^{14}\mathrm{N}(p,\gamma ){}^{15}\mathrm{O}$ reaction being the slowest process. Consequently, this reaction critically influences the solar composition, CNO neutrino fluxes, and the evolution of star clusters and galaxies. Recent direct measurements of ${}^{14}\mathrm{N}(p,\gamma ){}^{15}\mathrm{O}$ have reported an enhanced astrophysical $S$ factor. This work presents a microscopic theoretical study of the ${}^{14}\mathrm{N}(p,\gamma ){}^{15}\mathrm{O}$ reaction using the Gamow shell model in the coupled-channels representation. The calculations achieve good agreement with experimental data for both the total $S$ factors and the separate contributions from transitions to the ground state and excited states of ${}^{15}\mathrm{O}$. However, the predicted $S$ factor at zero energy exceeds the experimental value. Based on the computed $S$ factors, the derived carbon and nitrogen abundances align closely with predictions from recent ${}^{14}\mathrm{N}(p,\gamma ){}^{15}\mathrm{O}$ cross-section measurements, yet remain significantly lower than the latest solar neutrino observation values.

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• Nuclear astrophysics
• Nuclear reaction rates
• Radiative capture
• S-factor
• 6 ≤ A ≤ 19
• Many-body techniques
• Nuclear reactions