Formation of star clusters: Models and simulations

Abstract

AbstractRecent progress is reviewed in describing the physical processes of star cluster formation, from the viewpoint of theoretical models and numerical simulations. In many studies, supersonic turbulent flows structure the gas into a network of clumps, filaments, and cores. Self-gravity drives star formation, moderated by turbulence, magnetic fields, and stellar feedback. Recent models and simulations describe the core mass function, the protostar mass function, and the star-formation rate. Several simulations indicate similar protostar birthrates, a mass advantage for firstborn protostars, and accretion rates that are superthermal and nearly constant. Recently observed core-filament systems with sonic line widths and parsec lengths present challenges for turbulent models.