Abstract

The dust contain of young protoplanetary disks is of crucial interest. As a building material for pebbles, planetesimals, and planetary cores, dust is at the heart of planet formation scenarios. The increasing number of observations of young disks in the sub-millimeter wavelength or in scattered light reveals also many structures in the dust distribution, like asymmetries, gaps and bumps. Explaining these observations as well as and their confrontation with theoritical models drive a lot of efforts to improve the numerical models of disk evolution and dynamics. Thanks to several years of experience in multi-fluid simulations of these dusty protoplanetary disks, I will present new updates about how dust concentrations can rise due to the vorticity of the gas. When large scale vortices form because of different instabilities, they tend to accumulate dust, even very small grains, and change dramatically the distribution of solids on long timescales. Super Earth planets also generate zonal flows, and even a gap in the disk, which also trigger dust concentrations in the form of disk-wide rings, with dust-to-gas ratios above unity. I will show the details and the possibilities of this scenario, and its implications as a new path bridging different instabilities necessary for a robust planet formation model.