Planetesimal Formation by Gravitational Instability of a Porous-Dust Disk

Abstract

Recently it is proposed that porous icy dust aggregates are formed by pairwise accretion of dust aggregates beyond the snowline. We calculate the equilibrium random velocity of porous dust aggregates taking into account mutual gravitational scattering, collisions, gas drag, and turbulent stirring and scattering. We find that the disk of porous dust aggregates becomes gravitationally unstable as they evolve through gravitational compression in the minimum-mass solar nebula model for a reasonable range of turbulence strength, which leads to rapid formation of planetesimals.

arXiv comment14 pages, 5 figures, accepted for publication in ApJ Letters

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Cited by in corpus (8)

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• Planet Formation around Super Massive Black Holes in the Active Galactic Nuclei
• Formation of "Blanets" from Dust Grains around the Supermassive Black Holes in Galaxies
• Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Superparticle Method for Simulating Collisions
• Ejection of Chondrules from Fluffy Matrices
• Gravitational instability of a dust layer composed of porous silicate dust aggregates in a protoplanetary disk