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We study the dynamics and growth of dust particles in initially gravitationally unstable protoplanetary disks during the initial 1 Myr of disk evolution. We perform 2D hydrodynamical simulations of self-gravitating and viscous protoplanetary discs with the dust component using the FEOSAD code. Likewise, we consider the evolution of dust component including coagulation, fragmentation, momentum exchange with the gas, and self-gravity. We find that the level of turbulence in the disk strongly affects the dust evolution. Dust grows to the millimeter sizes in the disk with a viscosity parameter set to be α=10^−2, while in the disk with α=10^−4 pebbles a few cm in size are formed. We show that a ring structure, containing centimeter-sized pebbles, forms in the inner (2-6 au) disk when α=10^−4, due to the presence of a strong pressure bump there, caused by a significant viscosity transition. We find a close to linear correlation between the gas and pebble fluxes in the disk with α=10^−3, while in the disk with α=10^−4 deviation from the correlation exists due to the formation of ring structure. Our results demonstrate that the ring structure could possibly lead to the formation of planetesimals by the streaming instability and the early growth of embryos by pebble accretion.

Evolution of dust in gravitoviscous protoplanetary disks