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We have performed three-dimensional magneto-hydrodynamical simulations ofstellar accretion disks, using the PLUTO code, and studied the accretion of gasonto a Jupiter-mass planet and the structure of the circumplanetary gas flowafter opening a gap in the disk. We compare our results with simulations oflaminar, yet viscous disks with different levels of an $\alpha$-type viscosity.In all cases, we find that the accretion flow across the surface of the Hillsphere of the planet is not spherically or azimuthally symmetric, and ispredominantly restricted to the mid-plane region of the disk. Even in theturbulent case, we find no significant vertical flow of mass into the Hillsphere. The outer parts of the circumplanetary disk are shown to rotatesignificantly below Keplerian speed, independent of viscosity, while thecircumplanetary disk density (therefore the angular momentum) increases withviscosity. For a simulation of a magnetized turbulent disk, where the globalaveraged alpha stress is $\alpha_{MHD}=10^{-3}$, we find the accretion rateonto the planet to be $\dot{M}\approx 2\times10^{-6}M_{J}yr^{-1}$ for a gapsurface density of $12 g cm^{-2}$. This is about a third of the accretion rateobtained in a laminar viscous simulation with equivalent $\alpha$ parameter.

Accretion of gas onto gap-opening planets and circumplanetary flow structure in magnetized turbulent disks