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Substructures are ubiquitous in high resolution (sub-)millimeter continuumobservations of circumstellar disks. They are possibly caused by formingplanets embedded in the disk. To investigate the relation between observedsubstructures and young planets, we perform novel three-dimensional two-fluid(gas+1-mm-dust) hydrodynamic simulations of circumstellar disks with embeddedplanets (Neptune-, Saturn-, Jupiter-, 5 Jupiter-mass) at different orbitaldistances from the star (5.2AU, 30AU, 50AU). We turn these simulations intosynthetic (sub-)millimeter ALMA images. We find that all but the Neptune-massplanet open annular gaps in both the gas and the dust component of the disk. Wefind that the temporal evolution of the dust density distribution is distinctlydifferent of the gas'. For example, the planets cause significant verticalstirring of the dust in the circumstellar disk which opposes the verticalsettling. This creates a thicker dust disk than disks without a planet. We findthat this effect greatly influences the dust masses derived from the syntheticALMA images. Comparing the dust disk masses in the 3D simulations and the onesderived from the 2D ALMA synthetic images, we find the former to be a factor ofa few (up to 10) larger, pointing to that real disks might be significantlymore massive than previously thought based on ALMA continuum images using theoptically thin assumption and equation. Finally, we analyze the synthetic ALMAimages and provide an empirical relationship between the planet mass and thewidth of the gap in the ALMA images including the effects of the beam size.

First 3-D grid-based gas-dust simulations of circumstellar disks with an embedded planet