Formation of Massive Star Clusters by Fast H i Gas Collision

Young massive clusters (YMCs) are dense aggregates of young stars, which essential to galaxy evolution, owing their ultraviolet radiation, stellar winds, and supernovae. The typical mass radius YMCs M ∼ 104 M⊙ R 1 pc, respectively, indicating that many stars located in a small region. formation YMC precursor clouds may be difficult because very compact cloud should formed before feedback blows off the cloud. Recent observational studies suggest can as consequence fast H i gas collision with velocity ∼100 km s−1, is galaxy–galaxy interaction. In this study, we examine whether triggers using three-dimensional magnetohydrodynamics simulations, includes effects self-gravity, radiative cooling/heating, chemistry. We demonstrate gravitationally bound clumps > L 4 pc shock compressed region induced by collision, evolve into YMCs. Our results show precursors global gravitational collapse molecular clouds, even low-metal environments, such Magellanic Clouds. Additionally, cloud, 105 M⊙, created when consider explain origin cluster R136 system Large Cloud.