The ${}^{15}\mathrm{N}(n,\gamma ){}^{16}\mathrm{N}$ reaction plays a vital role in affecting the fluorine abundance produced in asymptotic giant branch stars and Wolf-Rayet stars by competing with the production reaction ${}^{15}\mathrm{N}(\alpha ,\gamma ){}^{19}\mathrm{F}$. However, the current understanding of this reaction is hampered by substantial discrepancies in both the neutron spectroscopic factors for the low-lying states of ${}^{16}\mathrm{N}$ and the reaction rate of ${}^{15}\mathrm{N}(n,\gamma ){}^{16}\mathrm{N}$. To address these uncertainties, we employ the Gamow shell model to investigate the spectroscopic factors of ${}^{16}\mathrm{N}$. Our results reveal that all these states are single-particle levels. Subsequently, the Gamow shell model coupled-channel representation was utilized to derive the cross section of ${}^{15}\mathrm{N}(n,\gamma ){}^{16}\mathrm{N}$ reaction at low energies. The associated reaction rate is then calculated based on the obtained cross section. Our calculation aligns with the available experimental data overall.

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• Nuclear astrophysics
• Nuclear reaction rates
• Nuclear reactions
• Radiative capture
• 6 ≤ A ≤ 19
• Optical, coupled-channel & distorted wave models