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The global evolution of protoplanetary disks (PPDs) has recently been shownto be largely controlled by the amount of poloidal magnetic flux threading thedisk, which is further controlled by the poorly understood process of magneticflux transport. In weakly ionized gas as in PPDs, magnetic flux is largelyfrozen in the electron fluid, except when resistivity is large. When the diskis largely laminar, we show that the relative drift between the electrons andions (the Hall-drift), and the ions and neutral fluids (ambipolar-drift) canplay a dominant role on the transport of magnetic flux. Using two-dimensionalsimulations that incorporate the Hall effect and ambipolar diffusion (AD) withprescribed diffusivities, we show that when large-scale poloidal field isaligned with disk rotation, the Hall effect rapidly drags magnetic flux inwardat the midplane region, while it slowly pushes flux outward above/below themidplane. This leads to a highly radially elongated field configuration as aglobal manifestation of the Hall-shear instability. This field configurationfurther promotes rapid outward flux transport by AD at the midplane, leading toinstability saturation. In quasi-steady state, magnetic flux is transportedoutward at approximately the same rate at all heights, and the rate iscomparable to the Hall-free case. For anti-aligned field polarity, the Halleffect consistently transports magnetic flux outward, leading to a largelyvertical field configuration in the midplane region. The field lines in theupper layer first bend radially inward and then outward to launch a disk wind.Overall, the net rate of outward flux transport is about twice faster than thealigned case. In addition, the rate of flux transport increases with increasingdisk magnetization. The absolute rate of transport is sensitive to diskmicrophysics which remains to be explored in future studies.

Hall-effect Mediated Magnetic Flux Transport in Protoplanetary Disks