Star formation in turbulent cloud cores with magnetic diffusion

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A molecular cloud core undergoes gravitational collapse to form a protostar and protoplanetary disk. Observations suggest that molecular cloud cores have magnetic field and turbulence. The magnetic field has a dissipative mechanism especially in the high-density gas.In this study, we investigated collapse of magnetized and turbulent molecular cloud cores, taking account of magnetic dissipation. We fallowed the evolution of the cloud cores from onset of collapse to formation of a protostar and protoplanetary disk, by using high-resolution adaptive mesh refinement (AMR) simulations. All the cloud cores produce protoplanetary disks irrespective of assumed strengths of magnetic field and turbulence. There is a tendency that a strong magnetic field model shows slower growth of a protoplanetary disk. The strong magnetic field models exhibit cavities in the infalling envelopes, which are caused by the interchange instability of the magnetic field.