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We use the Fokker-Planck equation and model the dispersive dynamics of solidparticles in annular protoplanetary disks whose gas component is more massivethan the particle phase. We model particle--gas interactions as hard spherecollisions, determine the functional form of diffusion coefficients, and showthe existence of two global unstable modes in the particle phase. These modeshave spiral patterns with the azimuthal wavenumber $m=1$ and rotate slowly. Weshow that in ring-shaped disks, the phase space density of solid particlesincreases linearly in time towards an accumulation point near the location ofpressure maximum, while instabilities grow exponentially. Therefore,planetesimals and planetary cores can be efficiently produced near the peaks ofunstable density waves. In this mechanism, particles migrating towards theaccumulation point will not participate in the formation of planets, and shouldeventually form a debris ring like the main asteroid belt or classical Kuiperbelt objects. We present the implications of global instabilities to theformation of ice giants and terrestrial planets in the solar system.

Global drag-induced instabilities in protoplanetary disks