  It has been considered that large satellites around gas planets form in-situ
circumplanetary discs (CPDs). However, dust particles supplied into CPDs drift
toward the central planets before they grow into satellitesimals, building
blocks of the satellites. We investigate the dust growth in laminar CPDs with
magnetic wind-driven accretion. In such laminar discs, dust particles can
settle onto the mid-plane and grow large by mutual collision more efficient
than in classical turbulent CPDs. First, we carry out 3D local MHD simulations
of a CPD including all the nonideal MHD effects (Ohmic resistivity, Hall effect
and ambipolar diffusion). We investigate if the disc accretion can be governed
by magnetic wind-driven accretion and how laminar the disc can be, in a
situation where the magnetic disc wind can be launched from the disc. Second,
we model 1D steady CPDs consistent with the results of the MHD simulations and
calculate the steady radial distributions of the dust profiles in the modeled
discs, taking account of the collisional growth, radial drift, fragmentation,
and vertical stirring by the Kelvin-Helmholtz instability. We show that
satellitesimals can form in such CPDs if the dust-to-gas mass ratio of the
inflow to the discs is larger than 0.02, which is 50 times smaller than the
critical value in turbulent CPDs. This condition can be satisfied when enough
amount of dust piles up at the gas pressure bump created by the planets. This
result shows that satellitesimals would form in laminar CPDs with magnetic
wind-driven accretion.
