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Dust gaps and rings appear ubiquitous in bright protoplanetary disks.Disk-planet interaction with dust-trapping at the edges of planet-induced gapsis one plausible explanation. However, the sharpness of some observed dustrings indicate that sub-mm-sized dust grains have settled to a thin layer insome systems. We test whether or not such dust around gas gaps opened byplanets can remain settled by performing three-dimensional, dust-plus-gassimulations of protoplanetary disks with an embedded planet. We find planetsmassive enough to open gas gaps stir small, sub-mm-sized dust grains to highdisk elevations at the gap edges, where the dust scale-height can reach ~70% ofthe gas scale-height. We attribute this dust 'puff-up' to the planet-inducedmeridional gas flows previously identified by Fung & Chiang and others. We thusemphasize the importance of explicit 3D simulations to obtain the verticaldistribution of sub-mm-sized grains around gas gaps opened by massive planets.We caution that the gas-gap-opening planet interpretation of well-defined dustrings is only self-consistent with large grains exceeding mm in size.

Puffed up Edges of Planet-opened Gaps in Protoplanetary Disks. I. hydrodynamic simulations