Abstract
Abstract 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 ${\rm N/O}$ ratios are similar to observed nitrogen-enriched galaxies (${\rm [N/O]}\gtrsim 0.5$). Then, once supernovae occur, the ${\rm N/O}$ 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 $\sim \!10^6$ M$_{\odot }$ 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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