Speaker
Description
By performing 3D radiation hydrodynamics simulations with radiative and stellar wind feedback, we study the formation of young massive star clusters (YMCs). We include the metal yield from stellar wind and supernovae. We find that the young massive star clusters are only born in the high-surface density clouds where radiative feedback becomes ineffective due to strong gravitational force from star clusters. In such a case, metal-enriched and high-density gas is formed around the star cluster. Before the supernovae occur, the high N/O ratios of gas are achieved due to stellar wind from Wolf-Rayet stars. The N/O ratios are comparable to that of discovered high-z galaxies (e.g., GN-z11). Also, some stars become nitrogen-enriched with N/O ratios similar to those of second-population stars in globular clusters (GCs). We show that metal-enriched stars are only born in star clusters more massive than 1.e6 Msun, estimating the conditions of YMC formation and metal yield due to stellar wind. These conditions of stellar multiple populations in YMCs allow us to constrain the formation site of GCs.
