Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation

Abstract

In our previous work (Paper I), we demonstrated that coagulation instability results in dust concentration against depletion due to the radial drift and accelerates dust growth locally. In this work (Paper II), we perform numerical simulations of coagulation instability taking into account effects of backreaction to gas and collisional fragmentation of dust grains. We find that the slowdown of the dust drift due to backreaction regulates dust concentration in the nonlinear growth phase of coagulation instability. The dust-to-gas surface density ratio increases from $10^{-3}$ up to $\sim 10^{-2}$. Each resulting dust ring tends to have mass of $\simeq 0.5M_{\oplus }-1.5M_{\oplus }$ in our disk model. In contrast to Paper I, the dust surface density profile shows a local plateau structure at each dust ring. In spite of the regulation at the nonlinear growth, the efficient dust concentration reduces their collision velocity. As a result, dust grains can grow beyond the fragmentation barrier, and the dimensionless stopping time reaches unity as in Paper I. The necessary condition for the efficient dust growth is (1) weak turbulence of $\alpha <1\times 10^{-3}$ and (2) a large critical velocity for dust fragmentation ($>1$ m/s). The efficient dust concentration in outer regions will reduce the inward pebble flux and is expected to decelerate the planet formation via the pebble accretion. We also find that the resulting rings can be unstable to secular gravitational instability (GI). The subsequent secular GI promotes planetesimal formation. We thus expect that a combination of these instabilities is a promising mechanism for dust-ring and planetesimal formation.

23 pages, 17 figures, accepted for publication in ApJ

References in corpus (45)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Protoplanetary Disk Structures in Ophiuchus
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Dust coagulation in protoplanetary disks: porosity matters
• Close-in planetesimal formation by pile-up of drifting pebbles
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• Planetesimal formation around the snow line in MRI-driven turbulent protoplanetary disks
• Thresholds for Particle Clumping by the Streaming Instability
• Can dust coagulation trigger streaming instability?
• A highly settled disk around Oph 163131
• Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks
• Streaming Instability for Particle-Size Distributions
• Sticking Properties of Silicates in Planetesimal Formation Revisited
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Ice Grain Collisions in Comparison: CO${}_2$, H${}_2$O and their Mixtures
• Dust settling against hydrodynamic turbulence in protoplanetary discs
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• How large are the monomers of dust aggregates in planet-forming disks?: Insights from quantitative optical and near-infrared polarimetry
• Streaming Instability with Multiple Dust Species: II. Turbulence and Dust-Gas Dynamics at Nonlinear Saturation
• Solving the Coagulation Equation by the Moments Method
• Rapid formation of Gas Giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores
• Non-linear Development of Secular Gravitational Instability in Protoplanetary Disks
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• Collisional Growth and Fragmentation of Dust Aggregates with Low Mass Ratios. I: Critical Collision Velocity for Water Ice
• Transmission Electron Microscopy Study of the Morphology of Ices Composed of H2O, CO2, and CO on Refractory Grains
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• Rocky Planetesimal Formation via Fluffy Aggregates of Nanograins
• Impact of Local Pressure Enhancements on Dust Concentration inTurbulent Protoplanetary Discs
• Polydisperse Streaming Instability II. Methods for solving the linear stability problem
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Coagulation Instability in Protoplanetary Disks: A Novel Mechanism Connecting Collisional Growth and Hydrodynamical Clumping of Dust Particles
• On dust-gas gravitational instabilities in protoplanetary discs
• On the non-axisymmetric fragmentation of rings generated by the Secular Gravitational Instability
• Planetesimal formation around the snow line: I. Monte Carlo simulations of silicate dust pile-up in a turbulent disk
• Dust Accumulation near the Magnetospheric Truncation of Protoplanetary Discs around T Tauri Stars
• Planetesimal Formation by Gravitational Instability of a Porous-Dust Disk
• Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I: First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii

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