Collapse-drived outflow in star-forming molecular cores

摘要

Dynamical collapses of magnetized molecular cloud cores are studied with magnetohydrodynamic simulations form the runaway collapse phase to the accretion phase. In the runaway collapse, a disk threaded by magnetic field lines is contracting owing to its self-gravity, and its evolution is well expressed by a self-similar solution. The central density increases greatly In a finite timescale and reaches a density at which an opaque core is formed at the center. After that, matter accretes to the newly formed core(accretion phase). In this stage, a rotationally supported disk is formed in a cloud core without magnetic fields.