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We carried out 3D dust+gas radiative hydrodynamic simulations of formingplanets. We investigated a parameter grid of Neptune-, Saturn-, Jupiter-, and 5Jupiter-mass planets at 5.2, 30, 50 AU distance from their star. We found thatthe meridional circulation \citep{Szulagyi14,FC16} drives a strong verticalflow for the dust as well, hence the dust is not settled in the midplane, evenfor mm-sized grains. The meridional circulation will deliver dust and gasvertically 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 gainis $10^{-6}$ to $10^{-8}$ $\rm{M_{Jup}/yr}$. The difference between the dustand gas accretion rates is smaller with decreasing planetary mass. In thevicinity of the planet, the mm-grains can get trapped easier than the gas,which means the circumplanetary disk might be enriched with solids incomparison to the circumstellar disk. We calculated the local dust-to-gas ratio(DTG) everywhere in the circumstellar disk and identified the altitude abovethe midplane where the DTG is 1, 0.1, 0.01, 0.001. The larger the planetarymass, the higher the mm-sized dust is delivered and a larger fraction of thedust disk is lifted by the planet. The stirring of mm-dust is negligible forNeptune-mass planets or below, but significant above Saturn-mass.

Meridional Circulation of Dust and Gas in the Circumstellar Disk: Delivery of Solids onto the Circumplanetary Region