Massive stars are significant sites for the weak s-process (ws-process). In metal-rich stars, \(^{22}\) Ne and \(^{16}\) O are, respectively, the main neutron source and poison for the ws-process. In metal-poor stars, however, the abundance of \(^{22}\) Ne is limited by metallicity, so the contribution of \(^{22}\) Ne( \(\alpha\) , n) \(^{25}\) Mg reaction on the s-process is smaller. Conversely, the \(^{17}\) O( \(\alpha\) , n) \(^{20}\) Ne reaction becomes more prominent in these stars because of the most abundant \(^{16}\) O at all metallicities. In this study, we calculated the evolution of four metal-poor stars ( \(Z=10^{-3}\) ) for the zero-age main-sequence (ZAMS) masses of \(M (\textrm{ZAMS})=\) 15, 20, 25, and 30 M \(_{\odot }\) to investigate the effect of reaction rates on the ws-process. We adopt the new \(^{17}\) O( \(\alpha\) , n) \(^{20}\) Ne and \(^{17}\) O( \(\alpha , \gamma\) ) \(^{21}\) Ne reaction rates suggested by Best et al. (2013) and \(^{22}\) Ne( \(\alpha\) , n) \(^{25}\) Mg and \(^{22}\) Ne( \(\alpha , \gamma\) ) \(^{26}\) Mg reaction rates from Wiescher et al. (2023). The yields of the s-process isotopes with the updated reaction rates are compared with the results using the default reaction rates from JINA REACLIB. We found that the new \(^{17}\) O+ \(\alpha\) reaction rates enhance the ws-process in all stages, whereas the new \(^{22}\) Ne+ \(\alpha\) reaction rates enhance the ws-process only in the C and Ne burning stages. Updating these new reaction rates would increase the production of ws-process isotopes by tens of times. We also note that for more massive stars, the enhancement by the new \(^{17}\) O+ \(\alpha\) reaction rates becomes more significant.
