  We carried out 3D dust+gas radiative hydrodynamic simulations of forming
planets. We investigated a parameter grid of Neptune-, Saturn-, Jupiter-, and 5
Jupiter-mass planets at 5.2, 30, 50 AU distance from their star. We found that
the meridional circulation \citep{Szulagyi14,FC16} drives a strong vertical
flow for the dust as well, hence the dust is not settled in the midplane, even
for mm-sized grains. The meridional circulation will deliver dust and gas
vertically onto the circumplanetary region, efficiently bridging over the gap.
The Hill-sphere accretion rates for the dust are $\sim10^{-8}$ to $10^{-10}$
$\rm{M_{Jup}/yr}$, increasing with planet-mass. For the gas component, the gain
is $10^{-6}$ to $10^{-8}$ $\rm{M_{Jup}/yr}$. The difference between the dust
and gas accretion rates is smaller with decreasing planetary mass. In the
vicinity of the planet, the mm-grains can get trapped easier than the gas,
which means the circumplanetary disk might be enriched with solids in
comparison to the circumstellar disk. We calculated the local dust-to-gas ratio
(DTG) everywhere in the circumstellar disk and identified the altitude above
the midplane where the DTG is 1, 0.1, 0.01, 0.001. The larger the planetary
mass, the higher the mm-sized dust is delivered and a larger fraction of the
dust disk is lifted by the planet. The stirring of mm-dust is negligible for
Neptune-mass planets or below, but significant above Saturn-mass.
