Effect of dust radial drift on viscous evolution of gaseous disk

Abstract

The total amount of dust (or "metallicity") and the dust distribution in protoplanetary disks are crucial for planet formation. Dust grains radially drift due to gas--dust friction, and the gas is affected by the feedback from dust grains. We investigate the effects of the feedback from dust grains on the viscous evolution of the gas, taking into account the vertical dust settling. The feedback from the grains pushes the gas outward. When the grains are small and the dust-to-gas mass ratio is much smaller than unity, the radial drift velocity is reduced by the feedback effect but the gas still drifts inward. When the grains are sufficiently large or piled-up, the feedback is so effective that forces the gas flows outward. Although the dust feedback is affected by dust settling, we found that the 2D approximation reasonably reproduces the vertical averaged flux of gas and dust. We also performed the 2D two-fluid hydrodynamic simulations to examine the effect of the feedback from the grains on the evolution of the gas disk. We show that when the feedback is effective, the gas flows outward and the gas density at the region within $\sim 10\ \mbox{AU}$ is significantly depleted. As a result, the dust-to-gas mass ratio at the inner radii may significantly excess unity, providing the environment where planetesimals are easily formed via, e.g., streaming instability. We also show that a simplified 1D model well reproduces the results of the 2D two-fluid simulations, which would be useful for future studies.

Accepted for publication in ApJ, 15 pages, 9 figures

References in corpus (13)

• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• A comparative study of disc-planet interaction
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Close-in planetesimal formation by pile-up of drifting pebbles
• Dust sedimentation and self-sustained Kelvin-Helmholtz turbulence in protoplanetary disk mid-planes. I. Radially symmetric simulations
• Can dust coagulation trigger streaming instability?
• Discovery of a Disk Gap Candidate at 20 AU in TW Hydrae
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Effects of dust feedback on vortices in protoplanetary disks
• Assembling the Building Blocks of Giant Planets around Intermediate Mass Stars
• An opening criterion for dust gaps in protoplanetary discs
• Vertical Shearing Instabilities in Radially Shearing Disks: The Dustiest Layers of the Protoplanetary Nebula

Cited by in corpus (8)

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• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Vortex instabilities triggered by low-mass planets in pebble-rich, inviscid protoplanetary discs
• Morphological signatures induced by dust back reaction in discs with an embedded planet
• Migrating Low-Mass Planets in Inviscid Dusty Protoplanetary Discs
• Termination of an inward migration of a gap-opening planet triggered by dust feedback