Three-dimensional Global Simulations of Type-II Planet–Disk Interaction with a Magnetized Disk Wind. I. Magnetic Flux Concentration and Gap Properties

Giant planets embedded in protoplanetary disks (PPDs) can create annulus density gaps around their orbits the type-II regime, potentially responsible for ubiquity of annular substructures observed PPDs. Despite substantial amount works studying planet migration and gap properties, they are almost exclusively conducted under viscous accretion disk framework. However, recent studies have established magnetized winds as primary driving evolution, which co-exist with turbulence from magneto-rotational instability (MRI) outer We conduct a series 3D global non-ideal magneto-hydrodynamic (MHD) simulations planet-disk interaction applicable to Our properly resolve MRI accommodate MHD wind. found that triggers poloidal magnetic flux concentration its orbit. The concentrated strongly enhances angular momentum removal gap, is along inclined field through strong outflow emanating surface outward gap. resulting planet-induced shape more similar an inviscid disk, while being much deeper, be understood simple inhomogeneous wind torque prescription. corotation region characterized by fast trans-sonic flow asymmetric azimuth about lacking horseshoe turns, meridional weakened. acting on generally drives inward migration, though rate affected presence neighboring stochastic, planet-free concentration.