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Context: It is well known that the so-called s-process is responsible for theproduction of neutron-rich trans-iron elements, that form the bulk of the"heavy nuclides" (i.e. nuclides more massive than the iron-group nuclei) in thesolar-system composition, considered as "standard of reference" dataset forcosmic abundances. In particular, the s-process produces about half of all thetrans-iron isotopes by moving along the "valley of stability" through a seriesof neutron capture reactions and beta decays. More than one s-process"component" (i.e. a nucleosynthesis event with a single set of physicalconditions like neutron exposure, initial abundances and neutron density) isrequired in order to explain the observed solar distribution of s-nucleiabundances. Current views on the subject suggest the existence of severalcomponents that, in terms of stellar environments, correspond to distinctcategories of stars in different evolutionary phases. Aims: The purpose of thechapter is to review the s-process nucleosynthesis occurring in massive stars(so-called weak component of s-process), pointing particular attention on therecent studies devoted to analyze how the uncertainties due to stellarevolution modeling and, specifically, due to convective overshooting affect theefficiency of this nucleosynthesis process.

The s-process nucleosynthesis in massive stars: current status and uncertainties due to convective overshooting