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The fate of metals ejected by young OB associations into the InterstellarMedium (ISM) is investigated numerically. In particular, we study theenrichment of the cold gas phase, which is the material that forms molecularclouds. Following previous work, the expansion and collision of two supershellsin a diffuse ISM is simulated, in this case also introducing an advectedquantity which represents the metals expelled by the young stars. We adopt thesimplest possible approach, not differentiating between metals coming fromstellar winds and those coming from supernovae. Even though the hot, diffusephase of the ISM receives a significant amount of metals from the stars, thecold phase is efficiently shielded, with very little metal enrichment.Significant enrichment of the cold ISM will therefore be delayed by at leastthe cooling time of this hot phase. No variations in cloud metallicity withdistance from the OB association or with direction are found, which means thatthe shell collision does little to enhance the metallicity of the cold clumps.We conclude that the stellar generation that forms out of molecular structures,triggered by shell collisions cannot be significantly enriched.

Delayed metal recycling in galaxies: the inefficiency of cold gas enrichment in colliding supershell simulations