Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I: First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii

Abstract

Our previous linear analysis presents a new instability driven by dust coagulation in protoplanetary disks. The coagulation instability has the potential to concentrate dust grains into rings and assist dust coagulation and planetesimal formation. In this series of papers, we perform numerical simulations and investigate nonlinear outcome of coagulation instability. In this paper (Paper I), we first conduct local simulations to demonstrate the existence of coagulation instability. Linear growth observed in the simulations is in good agreement with the previous linear analysis. We next conduct radially global simulations to demonstrate that coagulation instability develops during the inside-out disk evolution due to dust growth. To isolate the various effects on dust concentration and growth, we neglect effects of backreaction to a gas disk and dust fragmentation in Paper I. This simplified simulation shows that either of backreaction or fragmentation is not prerequisite for local dust concentration via the instability. In most runs with weak turbulence, dust concentration via coagulation instability overcomes dust depletion due to radial drift, leading to the formation of multiple dust rings. The nonlinear development of coagulation instability also accelerates dust growth, and the dimensionless stopping time ${\tau }_{\mathrm{s}}$ reaches unity even at outer radii (>10 au). Therefore, coagulation instability is one promising process to retain dust grains and to accelerate dust growth beyond the drift barrier.

19 pages, 12 figures, accepted for publication in ApJ

References in corpus (12)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• Planetesimal formation starts at the snow line
• Dust retention in protoplanetary disks
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Rapid formation of Gas Giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores
• Solving the Coagulation Equation by the Moments Method
• Non-linear Development of Secular Gravitational Instability in Protoplanetary Disks
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• On the non-axisymmetric fragmentation of rings generated by the Secular Gravitational Instability
• On the settling of small grains in dusty discs: analysis and formulas

Cited by in corpus (2)

• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• On Secular Gravitational Instability in Vertically Stratified Disks