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The contribution by massive stars (M > 9 solar masses) to the weak s-processcomponent of the solar system abundances is primarily due to the 22Ne neutronsource, which is activated near the end of helium-core burning. The residual22Ne left over from helium-core burning is then reignited during carbonburning, initiating further s-processing that modifies the isotopicdistribution. This modification is sensitive to the stellar structure and thecarbon burning reaction rate. Recent work on the 12C + 12C reaction suggeststhat resonances located within the Gamow peak may exist, causing a strongincrease in the astrophysical S-factor and consequently the reaction rate. Toinvestigate the effect of an increased rate, 25 solar mass stellar models withthree different carbon burning rates, at solar metallicity, were generatedusing the Geneva Stellar Evolution Code (GENEC) with nucleosynthesispost-processing calculated using the NuGrid Multi-zone Post-Processing Networkcode (MPPNP). The strongest rate caused carbon burning to occur in a largeconvective core rather than a radiative one. The presence of this largeconvective core leads to an overlap with the subsequent convectivecarbon-shell, significantly altering the initial composition of thecarbon-shell. In addition, an enhanced rate causes carbon-shell burningepisodes to ignite earlier in the evolution of the star, igniting the 22Nesource at lower temperatures and reducing the neutron density.

The effect of 12C + 12C rate uncertainties on the weak s-process component