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The formation of a circumstellar disk in collapsing cloud cores isinvestigated with three-dimensional magnetohydrodynamic simulations. We preparefour types of initial cloud having different density profiles and calculatetheir evolution with or without a sink. To investigate the effect of magneticdissipation on disk formation, the Ohmic dissipation is considered in somemodels. Calculations show that disk formation is very sensitive to both theinitial cloud configuration and the sink treatment. The disk size considerablydiffers in clouds with different density profiles even when the initial cloudshave almost the same mass-to-flux ratio. Only a very small disk (\sim 10 AU insize) appears in clouds with a uniform density profile, whereas a large disk(\sim 100 AU in size) forms in clouds with a Bonnor-Ebert density profile. Inaddition, a large sink accretion radius numerically impedes disk formationduring the main accretion phase and tends to foster the misleading notion thatdisk formation is completely suppressed by magnetic braking. The protostellaroutflow is also greatly affected by the sink properties. A sink accretionradius of \lesssim 1 AU and sink threshold density of \gtrsim 10^ 13 cm^-3 arenecessary for investigating disk formation during the main accretion phase.

Conditions for Circumstellar Disk Formation: Effects of Initial Conditions and Sink Treatment