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We present global hydrodynamic and magnetohydrodynamic (MHD) simulations withmesh refinement of accreting planets embedded in protoplanetary disks (PPDs).The magnetized disk includes Ohmic resistivity that depends on the overlyingmass column, leading to turbulent surface layers and a dead zone near themidplane. The main results are: (i) The accretion flow in the Hill sphere isintrinsically 3D for hydrodynamic and MHD models. Net inflow toward the planetis dominated by high latitude flows. A circumplanetary disk (CPD) forms. Itsmidplane flows outward in a pattern whose details differ between models. (ii)Gap opening magnetically couples and ignites the dead zone near the planet,leading to stochastic accretion, a quasi-turbulent flow in the Hill sphere anda CPD whose structure displays high levels of variability. (iii) Advection ofmagnetized gas onto the rotating CPD generates helical fields that launchmagnetocentrifugally driven outflows. During one specific epoch a highlycollimated, one-sided jet is observed. (iv) The CPD's surface density$\sim30{\rm\,g\,cm^{-2}}$, small enough for significant ionization andturbulence to develop. (v) The accretion rate onto the planet in the MHDsimulation reaches a steady value $8 \times 10^{-3} {\rm M_\oplus yr^{-1}}$,and is similar in the viscous hydrodynamic runs. Our results suggest that gasaccretion onto a forming giant planet within a magnetized PPD with dead zoneallows rapid growth from Saturnian to Jovian masses. As well as being relevantfor giant planet formation, these results have important implications for theformation of regular satellites around gas giant planets.

Global hydromagnetic simulations of a planet embedded in a dead zone: gap opening, gas accretion and formation of a protoplanetary jet