\begin{document}$ (\alpha,p)^{14} $\end{document}N among many others. We calculated the upper and lower limits of the 11C\begin{document}$ (\alpha,p)^{14} $\end{document}N rate by taking account of the low energy resonances above the threshold, which have not been included in the previous SN nucleosynthesis calculations. These resonance contributions significantly change the 11C abundance, which decays to 11B with a half-life of 20.34 m, and affects the resultant isotopic abundance ratio of 11B/10B at \begin{document}$ M_r=3.78-4.4M_{\odot} $\end{document} from which the presolar X grains could form. The 11B/10B isotopic ratio measured in X grains can help to understand the origin of solar system boron and constrain still unknown neutrino mass hierarchy if the observational and theoretical uncertainties associated with these abundances are reduced. We emphasize that the further precise experiment of measuring the 11C\begin{document}$ (\alpha,p)^{14} $\end{document}N reaction cross sections at the astrophysically interesting energies of Gamow window 0.23−1.24 MeV, which corresponds to the effective temperature \begin{document}$ T=0.2-1 $\end{document} GK, could clarify CCSN contribution to the solar 11B/10B ratio."> Implication of radioactive nuclear reaction <sup>11</sup>C(<i>α</i>, <i>p</i>)<sup>14</sup>N in Supernova <i>ν</i>-process nucleosynthesis -
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