We study metal enrichment originating from stellar wind and supernovae in low-metallicity clouds by performing three-dimensional radiation hydrodynamics simulations. We find that metals ejected from stellar wind are accumulated, leading to subsequent star formation in the nitrogen-enriched gas. During this early phase, the N/O ratios are similar to observed nitrogen-enriched galaxies ([N/O] 0.5). Then, once supernovae occur, the N/O ratios decrease significantly. If the duration of star formation is comparable to the time-scale of supernovae, the mass fraction of nitrogen-enriched stars reaches half the mass of star clusters. We suggest that the mass of the star cluster needs to exceed ~ \!10⁶ M to have multiple populations due to stellar wind, considering the condition for massive star cluster formation and the timescales of stellar evolution.
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Fukushima et al. (2024) studied this question.
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