Instabilities in dusty non-isothermal proto-planetary discs

Abstract

Protoplanetary discs (PPDs) can host a number of instabilities that may partake directly or indirectly in the process of planetesimal formation. These include the Vertical Shear Instability (VSI), Convective Overstability (COS), Streaming Instability (SI), and Dust Settling Instability (DSI), to name a few. Notably, the VSI and COS have mostly been studied in purely gaseous discs, while the SI and DSI have only been analyzed in isothermal discs. How these instabilities operate under more general conditions is therefore unclear. To this end, we devise a local model of a PPD describing a non-isothermal gas interacting with a single species of dust via drag forces. Using this, we find that dust drag sets minimum length scales below which the VSI and COS are suppressed. Similarly, we find that the SI can be suppressed on sufficiently small scales by the gas' radial buoyancy if it cools on roughly a dynamical timescale. We show that the DSI can be effectively stabilized by vertical buoyancy, except at special radial and vertical length scales. We also find novel instabilities unique to a dusty, non-isothermal gas. These result in a dusty analog of the COS that operates in slowly cooled discs, and a dusty version of the VSI that is strongly enhanced by dust settling. We briefly discuss the possible implications of our results on planetesimal formation.

arXiv comment40 pages, 26 figures

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Cited by in corpus (7)

• Polydisperse Formation of Planetesimals: The dust size distribution in clumps
• Resonant drag instabilities for polydisperse dust. II. The streaming and settling instabilities
• Filament formation due to diffusive instabilities in dusty protoplanetary disks
• Nonlinear Evolution of the Unstratified Polydisperse Dust Settling Instability
• Hydrodynamical simulations of the vertical shear instability with dynamic dust and cooling rates in protoplanetary disks
• Magnetic clumping of charged dust in the dense interstellar medium
• Streaming instabilities in accreting protoplanetary disks: A parameter study