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In the core-accretion model the nominal runaway gas-accretion phase bringsmost planets to multiple Jupiter masses. However, known giant planets arepredominantly Jupiter-mass bodies. Obtaining longer timescales for gasaccretion may require using realistic equations of states, or accounting forthe dynamics of the circumplanetary disk (CPD) in low-viscosity regime, orboth. Here we explore the second way using global, three-dimensional isothermalhydrodynamical simulations with 8 levels of nested grids around the planet. Inour simulations the vertical inflow from the circumstellar disk (CSD) to theCPD determines the shape of the CPD and its accretion rate. Even withoutprescribed viscosity Jupiter's mass-doubling time is $\sim 10^4$ years,assuming the planet at 5.2 AU and a Minimum Mass Solar Nebula. However, we showthat this high accretion rate is due to resolution-dependent numericalviscosity. Furthermore, we consider the scenario of a layered CSD, viscous onlyin its surface layer, and an inviscid CPD. We identify two planet-accretionmechanisms that are independent of the viscosity in the CPD: (i) the polarinflow -- defined as a part of the vertical inflow with a centrifugal radiussmaller than 2 Jupiter-radii and (ii) the torque exerted by the star on theCPD. In the limit of zero effective viscosity, these two mechanisms wouldproduce an accretion rate 40 times smaller than in the simulation.

Accretion of Jupiter-mass Planets in the Limit of Vanishing Viscosity