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.

14 pages, 5 figures, accepted for publication in ApJ Letters

References in corpus (2)

• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• $N$-body Simulation of Planetesimal Formation Through Gravitational Instability of a Dust Layer

Cited by in corpus (5)

• Planet Formation around Super Massive Black Holes in the Active Galactic Nuclei
• Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk
• Ejection of Chondrules from Fluffy Matrices
• Superparticle Method for Simulating Collisions
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation