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As accretion in protoplanetary disks is enabled by turbulent viscosity, theborder between active and inactive (dead) zones constitutes a location wherethere is an abrupt change in the accretion flow. The gas accumulation thatensues triggers the Rossby wave instability, that in turn saturates intoanticyclonic vortices. It was suggested that the trapping of solids within themleads to a burst of planet formation on very short timescales. We performtwo-dimensional global simulations of the dynamics of gas and solids in anon-magnetized thin protoplanetary disk with the Pencil Code. We use multipleparticle species of radius 1, 10, 30, and 100 cm, solving for the particles'gravitational interaction by a particle-mesh method. The dead zone is modeledas a region of low viscosity. Adiabatic and locally isothermal equations ofstate are used. We find that the Rossby wave instability is triggered under avariety of conditions, thus making vortex formation a robust process. Insidethe vortices, fast accumulation of solids occurs and the particles collapseinto objects of planetary mass in timescales as short as five orbits. Becausethe drag force is size-dependent, aerodynamical sorting ensues within thevortical motion, and the first bound structures formed are composed primarilyof similarly-sized particles. In addition to erosion due to ram pressure, weidentify gas tides from the massive vortices as a disrupting agent of formedprotoplanetary embryos. We also estimate the collisional velocity history ofthe particles that compose the most massive embryo by the end of thesimulation, finding that the vast majority of them never experienced acollision with another particle at speeds faster than 1 m/s.

Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks