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The formation of circumstellar disks is investigated using three-dimensionalresistive magnetohydrodynamic simulations, in which the initial prestellarcloud has a misaligned rotation axis with respect to the magnetic field. Weexamine the effects of (i) the initial angle difference between the globalmagnetic field and the cloud rotation axis ($\theta_0$) and (ii) the ratio ofthe thermal to gravitational energy ($\alpha_0$). We study $16$ models in totaland calculate the cloud evolution until $\sim \! 5000$ yr after protostarformation. Our simulation results indicate that an initial non-zero $\theta_0$($> 0$) promotes the disk formation but tends to suppress the outflow driving,for models that are moderately gravitationally unstable, $\alpha_0 \lesssim 1$.In these models, a large-sized rotationally-supported disk forms and a weakoutflow appears, in contrast to a smaller disk and strong outflow in thealigned case ($\theta_0 = 0$). Furthermore, we find that when the initial cloudis highly unstable with small $\alpha_0$, the initial angle difference$\theta_0$ does not significantly affect the disk formation and outflowdriving.

The Effect of Misalignment between Rotation Axis and Magnetic Field on Circumstellar Disk