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

Abstract

Stellar winds of massive ($\gtrsim 9{\mathrm{M}}_{\odot }$) and very massive ($\gtrsim 100{\mathrm{M}}_{\odot }$) stars may play an important role in the metal-enrichment during the formation of star clusters. With novel high-resolution hydrodynamical \textsc{griffin}-project simulations, we investigate the rapid recycling of stellar wind-material during the formation of massive star clusters up to $M_{\mathrm{cluster}}\sim 2\times 10^5{\mathrm{M}}_{\odot }$ in a low-metallicity dwarf galaxy starburst. The simulation realises new stars from a stellar initial mass function (IMF) between $0.08{\mathrm{M}}_{\odot }$ and $\sim 400{\mathrm{M}}_{\odot }$ and follows stellar winds, radiation and supernova-feedback of single massive stars with evolution tracks. Star clusters form on timescales less than $\sim 5$ 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 ($\gtrsim 10^4{\mathrm{M}}_{\odot }$) and the locked wind-material increases approximately as $M_{\mathrm{cluster}}^2$. 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 $M_{\mathrm{cluster}}=10^7{\mathrm{M}}_{\odot }$ 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.

24 pages, 22 figures, updated to match the version accepted for publication in MNRAS

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