Impacts of stellar wind and supernovae on star cluster formation: Origins of extremely high N/O ratios and multiple stellar populations

Fukushima, Hajime,   & Yajima, Hidenobu

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 N∕O ratios are similar to observed nitrogen-enriched galaxies ([N∕O]rsim0.5). 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.