Star clusters forming in a low metallicity starburst -- rapid self-enrichment by (very) massive stars

Stellar winds of massive (9\,M_) and very massive (100\,M_) stars may play an important role in the metal-enrichment during the formation of star clusters. With novel high-resolution hydrodynamical {griffin}-project simulations, we investigate the rapid recycling of stellar wind-material during the formation of massive star clusters up to Mcluster~2×10⁵\,M_ in a low-metallicity dwarf galaxy starburst. The simulation realises new stars from a stellar initial mass function (IMF) between 0.08\,M_ and ~400\,M_ and follows stellar winds, radiation and supernova-feedback of single massive stars with evolution tracks. Star clusters form on timescales less than ~5 Myr, and their supernova-material is very inefficiently recycled. Stellar wind-material, however, is trapped in massive clusters resulting in the formation of stars self-enriched in Na, Al, and N within only a few Myr. Wind-enriched (second population) stars can be centrally concentrated in the most massive clusters (10⁴\,M_) and the locked wind-material increases approximately as Mcluster². These trends resemble the characteristics of observed second population stars in globular clusters. We fit scaling relations to the log-normal distributed wind-mass fractions and extrapolate to possible globular cluster progenitors of Mcluster=10⁷\,M_ to investigate whether a dominant second population could form. This can only happen if the IMF is well sampled, single massive stars produce at least a factor of a few more enriched winds e.g. through a top-heavy IMF, and a significant fraction of the first population (unenriched) stars is lost during cluster evolution.