Linear growth of streaming instability in pressure bumps

Abstract

Streaming instability is a powerful mechanism which concentrates dust grains in pro- toplanetary discs, eventually up to the stage where they collapse gravitationally and form planetesimals. Previous studies inferred that it should be ineffective in viscous discs, too efficient in inviscid discs, and may not operate in local pressure maxima where solids accumulate. From a linear analysis of stability, we show that streaming instability behaves differently inside local pressure maxima. Under the action of the strong differential advection imposed by the bump, a novel unstable mode develops and grows even when gas viscosity is large. Hence, pressure bumps are found to be the only places where streaming instability occurs in viscous discs. This offers a promising way to conciliate models of planet formation with recent observations of young discs.

11 pages, 17 figures, accepted for publication in MNRAS

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• Physical models of streaming instabilities in protoplanetary disks
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• Pebble drift and planetesimal formation in protoplanetary discs with embedded planets
• Vortex-like kinematic signal, spirals, and beam smearing effect in the HD 142527 disk
• Stratified and vertically-shearing streaming instabilities in protoplanetary disks
• The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks: Planetesimal formation thresholds explored in two-dimensional global models
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
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• Turbulent Dust-trapping Rings as Efficient Sites for Planetesimal Formation
• Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
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• Channels for streaming instability in dusty discs
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• Experimental study of clusters in dense granular gas and implications for the particle stopping time in protoplanetary disks
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