Ring Morphology with Dust Coagulation in Protoplanetary Disks

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.

arXiv comment11 pages, 5 figures, accepted for publication in ApJL on 21 December 2019

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Cited by in corpus (7)

• Distribution of solids in the rings of the HD 163296 disk: a multiwavelength study
• The Preservation of Super Earths and the Emergence of Gas Giants after Their Progenitor Cores have Entered the Pebble Isolation Phase
• Planet-induced Vortices with Dust Coagulation in Protoplanetary Disks
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