Establishing Dust Rings and Forming Planets Within Them

Abstract

Radio images of protoplanetary disks demonstrate that dust grains tend to organize themselves into rings. These rings may be a consequence of dust trapping within gas pressure maxima wherein the local high dust-to-gas ratio is expected to trigger the formation of planetesimals and eventually planets. We revisit the behavior of dust near gas pressure perturbations enforced by a planet in two-dimensional, shearing box simulations. While dust grains collect into generally long-lived rings, particles with small Stokes parameter ${\tau }_s<0.1$ tend to advect out of the ring within a few drift timescales. Scaled to the properties of ALMA disks, we find that rings composed of larger particles (${\tau }_s\ge 0.1$) can nucleate a dust clump massive enough to trigger pebble accretion which proceeds to ingest the entire dust ring well within $\sim$1 Myr. To ensure the survival of the dust rings, we favor a non-planetary origin and typical grain size ${\tau }_s\lesssim 0.05$--0.1. Planet-driven rings may still be possible but if so we would expect the orbital distance of the dust rings to be larger for older systems.

To appear in ApJ. Paper refocused to forcing by a planet

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• The compositions of the HR 8799 planets reflect accretion of both solids and metal-enriched gas
• Jupiter-like uniform metal enrichment in a system of multiple giant exoplanets
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• The Dissolution of Planetesimals in Electrostatic Fields
• Planetesimal formation at the gas pressure bump following a migrating planet II. Effects of dust growth