Gravitational Collapse in Filaments, Clumps, and Cores: 3D Simulations of Hydrodynamic Turbulence

We discuss 3D simulations of turbulent, self-gravitating gas designed to study the formation and collapse of molecular cloud cores in young star clusters. Clusters rather than isolated objects form when the turbulent damping time exceeds the free-fall time in a clump. We find that a variety of core density profiles are produced including Bonner-Ebert spheres as well as logatropes. The core mass and angular momentum distributions match the observations.