  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 (Szulagyi et al. 2014, Fung & Chiang 2016) 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 planet vicinity, 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 is 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. We also
examined the formation of dust rings (similar to ALMA observations) and we
found that they are formed by the merging of the spiral arms of planets.
