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

Abstract

The formation of circumstellar disks is investigated using three-dimensional resistive magnetohydrodynamic simulations, in which the initial prestellar cloud has a misaligned rotation axis with respect to the magnetic field. We examine the effects of (i) the initial angle difference between the global magnetic field and the cloud rotation axis (${\theta }_0$) and (ii) the ratio of the thermal to gravitational energy (${\alpha }_0$). We study $16$ models in total and calculate the cloud evolution until $\sim 5000$ yr after protostar formation. 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 weak outflow appears, in contrast to a smaller disk and strong outflow in the aligned case (${\theta }_0=0$). Furthermore, we find that when the initial cloud is highly unstable with small ${\alpha }_0$, the initial angle difference ${\theta }_0$ does not significantly affect the disk formation and outflow driving.

arXiv comment27 pages, 21 figures, 2 tables, Accepted for publication in ApJ

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