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The $s$-process in massive stars produces the weak component of the$s$-process (nuclei up to $A \sim 90$), in amounts that match solar abundances.For heavier isotopes, such as barium, production through neutron capture issignificantly enhanced in very metal-poor stars with fast rotation. However,detailed theoretical predictions for the resulting final $s$-process abundanceshave important uncertainties caused both by the underlying uncertainties in thenuclear physics (principally neutron capture reaction and $\beta$-decay rates)as well as by the stellar evolution modeling. In this work, we investigated theimpact of nuclear-physics uncertainties relevant to the $s$-process in massivestars. Using a Monte-Carlo based approach, we performed extensive nuclearreaction network calculations that include newly evaluated upper and lowerlimits for the individual temperature dependent reaction rates. We found thatmost of the uncertainty in the final abundances is caused by uncertainties inthe neutron capture rates, while $\beta$-decay rate uncertainties affect only afew nuclei near $s$-process branchings. The $s$-process in rotating metal-poorstars shows quantitatively different uncertainties and key reactions, althoughthe qualitative characteristics are similar. We confirmed that our results donot significantly change at different metallicities for fast rotating massivestars in the very low metallicity regime. We highlight which of the identifiedkey reactions are realistic candidates for improved measurement by futureexperiments.

Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations