Cosmic implications of the <inline-formula><tex-math id="M1">\begin{document}${^{12}{\bf C}(\boldsymbol n,\bf\gamma)^{13}{\bf C} }$\end{document}</tex-math><alternatives><graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="//www.macurncorp.com/hepnp/article/app/id/4ac88d36-cd32-4a82-a3d8-f4c7eb511494/CPC-2023-0413_M1.jpg"/><graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="//www.macurncorp.com/hepnp/article/app/id/4ac88d36-cd32-4a82-a3d8-f4c7eb511494/CPC-2023-0413_M1.png"/></alternatives></inline-formula> reaction: a nuclear astrophysical perspective -

\begin{document}$ ^{12}\mathrm C $\end{document} within the relevant astrophysical energy range. Through rigorous R-matrix analysis, we determined the Maxwellian-averaged cross section to be 11.98

\begin{document}$ \pm $\end{document}

0.25 μb at kT = 30 keV. This result is approximately four times higher than the thermal neutron capture cross section estimated in earlier studies assuming the

\begin{document}$ \dfrac{1}{v} $\end{document}

law. The implications of our findings extend to the region of inhomogeneous Big-Bang models in nuclear astrophysics, where understanding the behaviour of neutron capture cross sections plays a crucial role in elucidating the intricate processes that shaped the early universe."> Cosmic implications of the <inline-formula><tex-math id="M1">\begin{document}${^{12}{\bf C}(\boldsymbol n,\bf\gamma)^{13}{\bf C} }$\end{document}</tex-math><alternatives><graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="//www.macurncorp.com/hepnp/article/app/id/4ac88d36-cd32-4a82-a3d8-f4c7eb511494/CPC-2023-0413_M1.jpg"/><graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="//www.macurncorp.com/hepnp/article/app/id/4ac88d36-cd32-4a82-a3d8-f4c7eb511494/CPC-2023-0413_M1.png"/></alternatives></inline-formula> reaction: a nuclear astrophysical perspective -

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