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Transition disks have dust-depleted inner regions and may represent anintermediate step of an on-going disk dispersal process, where planet formationis probably in progress. Recent millimetre observations of transition disksreveal radially and azimuthally asymmetric structures, where micron- andmillimetre-sized dust particles may not spatially coexist. These properties canbe the result of particle trapping and grain growth in pressure bumpsoriginating from the disk interaction with a planetary companion. The multiplefeatures observed in some transition disks, such as SR 21, suggest the presenceof more than one planet. We study the gas and dust distributions of a diskhosting two massive planets as function of different disk and dust parameters.Observational signatures, such as the spectral energy distribution,sub-millimetre, and polarised images are simulated for the various parameters.We confirm that planets can lead to particle trapping, although for a disk withhigh viscosity ($\alpha_{\rm{turb}}=10^{-2}$), the planet should be moremassive than $5 M_{\rm{Jup}}$ and dust fragmentation should occur with lowefficiency ($v_{f}\sim30\rm{m s}^{-1}$). This will lead to a ring-like featureas observed in transition disks in the millimetre. When trapping occurs, wefind that a smooth distribution of micron sized grains throughout the disk,sometimes observed in scattered light, can only happen if the combination ofplanet mass and turbulence is such that small grains are not fully filteredout. A high disk viscosity ($\alpha_{\rm{turb}}=10^{-2}$) ensures areplenishment of the cavity in micron-sized dust, while for lower viscosity($\alpha_{\rm{turb}}=10^{-3}$), the planet mass is constrained to be less than$5 M_{\rm{Jup}}$. In these cases, the gas distribution is likely to showlow-amplitude azimuthal asymmetries caused by disk eccentricity rather than bylong-lived vortices.

Gas and dust structures in protoplanetary disks hosting multiple planets