Princeton University Wunch Talk

ABSTRACT: Star formation in collapsing molecular cloud cores has been well studied so far. It is a very complicated process which involves many physical processes such as self-gravity, magnetohydrodynamics, radiation transfer, chemical reactions, non-ideal MHD effects, and so on. We perform 3D nested-grid radiation magnetohydrodynamic simulations of formation of protostellar cores from molecular cloud cores with and without Ohmic dissipation. Magnetic fields transport angular momentum so efficiently that circumstellar disks cannot be formed in the ideal MHD models, but Ohmic dissipation enables circumstellar disk formation by reducing magnetic flux and suppressing angular momentum transport. We also show that two different outflows are naturally launched; slow loosely-collimated outflow from first cores and fast well-collimated jet from protostellar cores.