\begin{document}$ ^{12} {\rm{C}}$\end{document}\begin{document}$ (\nu_{e},e^{-})^{12} {\rm{N}} _{\rm{g.s.}} $\end{document}, \begin{document}$ ^{16} {\rm{O}}$\end{document}\begin{document}$ (\nu_{e},e^{-})^{16} {\rm{F}}$\end{document}, \begin{document}$ ^{56} {\rm{Fe}}$\end{document}\begin{document}$ (\nu_{e},e^{-})^{56} {\rm{C}}{\rm{o}}$\end{document}, and \begin{document}$ ^{208} {\rm{Pb}}$\end{document}\begin{document}$ (\nu_{e},e^{-})^{208} {\rm{Bi}}$\end{document} reactions are consistent with those predicted using the QRPA, Hybrid, RPA, and pnQRPA models within an order of magnitude. These results are reasonable given our current knowledge of neutrino-nucleus reactions. Building on this foundation, we propose a semi-empirical parametrization formula that describes the spectrum-weighted cross section of supernova neutrinos as a function of neutrino effective temperature. This formula is instrumental in the development of a convenient database for neutrino-nucleus reaction cross sections. Such a database is anticipated to streamline the process of accessing cross section data, thereby enhancing the efficiency of model calculations based on nuclear astrophysical networks."> Neutrino-nucleus reaction cross sections in supernova explosion -
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