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The abundances of elements in stars are a critical clue to their origins.Observed star-to-star variations in logarithmic abundance within an opencluster are typically only $\sim 0.01-0.05$ over many elements, significantlysmaller than the variation of $\sim 0.06-0.3$ seen in the interstellar mediumfrom which the stars form. It is unknown why clusters are so homogenous, andwhether homogeneity should also prevail in regions of lower star formationefficiency that do not produce bound clusters. Here we report adaptive meshsimulations using passively-advected scalars in order to trace the mixing ofchemical elements as star-forming clouds form and collapse. We show thatturbulent mixing during cloud assembly naturally produces a stellar abundancescatter at least ~5 times smaller than that in the gas, sufficient to fullyexplain the observed chemical homogeneity of stars. Moreover, mixing occursvery early, so that regions with efficiencies $\varepsilon \sim 10\%$ arenearly as well-mixed as those with $\varepsilon\sim 50\%$. This implies thateven regions that do not form bound clusters are likely to be well-mixed, andenhances the prospects for using chemical tagging to reconstruct dissolved starclusters via their unique chemical signatures.

Early turbulent mixing as the origin of chemical homogeneity in open star clusters