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Recently it is proposed that porous icy dust aggregates are formed bypairwise accretion of dust aggregates beyond the snowline. We calculate theequilibrium random velocity of porous dust aggregates taking into accountmutual gravitational scattering, collisions, gas drag, and turbulent stirringand scattering. We find that the disk of porous dust aggregates becomesgravitationally unstable as they evolve through gravitational compression inthe minimum-mass solar nebula model for a reasonable range of turbulencestrength, which leads to rapid formation of planetesimals.

Planetesimal Formation by Gravitational Instability of a Porous-Dust Disk