Ring Morphology with Dust Coagulation in Protoplanetary Disks
arXiv:1912.11178 · doi:10.3847/2041-8213/ab65c6
Abstract
Tidal interactions between the embedded planets and their surrounding protoplanetary disks are often postulated to produce the observed complex dust substructures, including rings, gaps, and asymmetries. In this Letter, we explore the consequences of dust coagulation on the dust dynamics and ring morphology. Coagulation of dust grains leads to dust size growth which, under typical disk conditions, produces faster radial drifts, potentially threatening the dust ring formation. Utilizing 2D hydrodynamical simulations of protoplanetary disks which include a full treatment of dust coagulation, we find that if the planet does not open a gap quickly enough, the formation of an inner ring is impeded due to dust coagulation and subsequent radial drift. Furthermore, we find that a "buildup" of sub-mm sized grains often appears in the dust emission at the outer edge of the dust disk.
11 pages, 5 figures, accepted for publication in ApJL on 21 December 2019
References in corpus (13)
- Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
- Gas- and dust evolution in protoplanetary disks
- Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
- Closed-form expressions for particle relative velocities induced by turbulence
- Structure and evolution of pre-main sequence circumstellar disks
- Multiple Disk Gaps and Rings Generated by a Single Super-Earth
- Survival of the mm-cm size grain population observed in protoplanetary disks
- Type I Planet Migration in Nearly Laminar Disks
- Effects of dust feedback on vortices in protoplanetary disks
- Including Dust Coagulation in Hydrodynamic Models of Protoplanetary Disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet
- On the planetary interpretation of multiple gaps and rings in protoplanetary disks seen by ALMA
- Long-Lived Dust Asymmetries at Dead Zone Edges in Protoplanetary Disks
- Effects of Ringed Structures and Dust Size Growth on Millimeter Observations of Protoplanetary Disks