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We perform a series of 3D simulations to study the accretion of giant planetembedded in protoplanetary discs (PPDs) over gap-opening timescales. We findthat the accretion mass flux mainly comes from the intermediate latitude abovethe disc midplane. The circumplanetary disc (CPD) for a super-thermal planet isrotation-supported up to $\sim$20-30\% of the planet Hill radius. While bothmass inflow and outflow exists in the CPD midplane, the overall trend is anoutflow that forms a meridional circulation with high-latitude inflows. Weconfirm the absence of accretion outburst from disc eccentricity excited bymassive planets in our 3D simulations, contrary to the consensus of previous 2Dsimulations. This suggests the necessity of 3D simulations of accretion evenfor super-Jupiters. The accretion rates of planets measured in steady-state canbe decomposed into the ``geometric" and ``density depletion" factors. Throughextensive parameter survey, we identify a power-law scaling for the geometricfactor $\propto q_{\rm th}^{2/3}$ for super-thermal planets ($q_{\rm th}$ beingthe thermal mass ratio), which transforms to $\propto q_{\rm th}^{2}$ for lessmassive cases. The density depletion factor is limited by the disc accretionrate for mildly super-thermal planets, and by gap-opening for highlysuper-thermal ones. Moderate planetary eccentricities can enhance the accretionrates by a factor of $2-3$ through making the gap shallower, but does notimpact the flow geometry. We have applied our simulations results to accretingprotoplanet system PDS 70 and can satisfactorily explain the accretion rate andCPD size in observations.

3D Global Simulations of Accretion onto Gap-opening Planets: Implications for Circumplanetary Disc Structures and Accretion Rates