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The structure and evolution of protoplanetary disks (PPDs) are largelygoverned by disk angular momentum transport, mediated by magnetic fields. Inthe most observable outer disk, PPD gas dynamics is primarily controlled byambipolar diffusion as the dominant non-ideal magnetohydrodynamic (MHD) effect.In this work, we study the gas dynamics in outer PPDs by conducting a set ofglobal 3D non-ideal MHD simulations with ambipolar diffusion and net poloidalmagnetic flux, using the Athena++ MHD code, with resolution comparable to localsimulations. Our simulations demonstrate the co-existence of magnetized diskwind and turbulence driven by the magneto-rotational instability (MRI). WhileMHD wind dominates disk angular momentum transport, the MRI turbulence alsocontributes significantly. We observe that magnetic flux spontaneouslyconcentrate into axisymmetric flux sheets, leading to radial variations inturbulence levels, stresses, and accretion rates. Annular substructures ariseas a natural consequence of magnetic flux concentration. The flux concentrationphenomena show diverse properties with different levels of disk magnetizationand ambipolar diffusion. The disk generally loses magnetic flux over time,though flux sheets could prevent the leak of magnetic flux in some cases. Ourresults demonstrate the ubiquity of disk annular substructures in weakly MRIturbulent outer PPDs, and imply a stochastic nature of disk evolution.

Global Three-Dimensional Simulations of Outer Protoplanetary Disks with Ambipolar Diffusion