Minimum Dust Abundances for Planetesimal Formation via Secular Gravitational Instabilities

Abstract

We estimate minimum dust abundances required for secular gravitational instability (SGI) to operate at the midplane dust layer of protoplanetary disks. For SGI to be a viable process, the growth time of the instability T_grow must be shorter than the radial drift time of the dust T_drift. The growth time depends on the turbulent diffusion parameter alpha, because the modes with short wavelengths are stabilized by turbulent diffusion. Assuming that turbulence is excited via the Kelvin-Helmholtz or streaming instabilities in the dust layer, and that its strength is controlled by the energy supply rate from dust accretion, we estimate the diffusion parameter and the growth time of the instability. The condition T_grow < T_drift requires that the dust abundance must be greater than a critical abundance Z_min, which is a function of the Toomre parameter Q_g and aspect ratio h_g / r of the gas disk. For a wide range of parameter space, the required dust abundance is less than 0.1. A slight increase in dust abundance opens a possible route for the dust to directly collapse to planetesimals.

Accepted to the Astrophysical Journal

References in corpus (7)

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• From Planetesimal to Planet in Turbulent Disks. II. Formation of Gas Giant Planets
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• On Secular Gravitational Instability in Vertically Stratified Disks
• Drag-driven instability of a dust layer in a magnetized protoplanetary disc