Electrostatic Barrier against Dust Growth in Protoplanetary Disks. II. Measuring the Size of the "Frozen" Zone

Abstract

Coagulation of submicron-sized dust grains into porous aggregates is the initial step of dust evolution in protoplanetary disks. Recently, it has been pointed out that negative charging of dust in the weakly ionized disks could significantly slow down the coagulation process. In this paper, we apply the growth criteria obtained in Paper I to finding out a location ("frozen" zone) where the charging stalls dust growth at the fractal growth stage. For low-turbulence disks, we find that the frozen zone can cover the major part of the disks at a few to 100 AU from the central star. The maximum mass of the aggregates is approximately 10^{-7} g at 1 AU and as small as a few monomer masses at 100 AU. Strong turbulence can significantly reduce the size of the frozen zone, but such turbulence will cause the fragmentation of macroscopic aggregates at later stages. We examine a possibility that complete freezeout of dust evolution in low-turbulence disks could be prevented by global transport of dust in the disks. Our simple estimation shows that global dust transport can lead to the supply of macroscopic aggregates and the removal of frozen aggregates on a timescale of 10^6 yr. This overturns the usual understanding that tiny dust particles get depleted on much shorter timescales unless collisional fragmentation is effective. The frozen zone together with global dust transport might explain "slow" (\sim 10^6 yr) dust evolution suggested by infrared observation of T Tauri stars and by radioactive dating of chondrites.

14 pages, 13 figures, accepted for publication in ApJ

References in corpus (13)

• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Closed-form expressions for particle relative velocities induced by turbulence
• Towards planetesimals: dense chondrule clumps in the protoplanetary nebula
• Dust settling in local simulations of turbulent protoplanetary disks
• Numerical Modeling of the Coagulation and Porosity Evolution of Dust Aggregates
• Protoplanetary Disk Winds by Magnetorotational Instability : Formation of an Inner Hole and a Crucial Assist for Planet Formation
• Dust retention in protoplanetary disks
• Dead Zone Accretion Flows in Protostellar Disks
• High Velocity Dust Collisions: Forming Planetesimals in a Fragmentation Cascade with Final Accretion
• Collisional evolution of dust aggregates. From compaction to catastrophic destruction
• Electrostatic Barrier against Dust Growth in Protoplanetary Disks. I. Classifying the Evolution of Size Distribution

Cited by in corpus (33)

• A simple model for the evolution of the dust population in protoplanetary disks
• Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
• Modeling Magnetorotational Turbulence in Protoplanetary Disks with Dead Zones
• Dust growth and evolution in protoplanetary disks
• Particle Trapping and Streaming Instability in Vortices
• Electrostatic Barrier against Dust Growth in Protoplanetary Disks. I. Classifying the Evolution of Size Distribution
• Explaining millimeter-sized particles in brown dwarf disks
• Dust trapping by spiral arms in gravitationally unstable protostellar discs
• Charging of Aggregate Grains in Astrophysical Environments
• Charging and coagulation of dust in protoplanetary plasma environments
• The Physics of Protoplanetesimal Dust Agglomerates. Vi. Erosion of Large Aggregates as a Source of Micrometer-Sized Particles
• Growth and fragmentation of centimetre-sized dust aggregates: the dependence on aggregate size and porosity
• On the millimetre continuum flux-radius correlation of proto-planetary discs
• The Evolution of Protoplanetary Disks in the Arches Cluster
• Ionization and Dust Charging in Protoplanetary Disks
• Formation of Comets
• Measurement of net electric charge and dipole moment of dust aggregates in a complex plasma
• Disc population synthesis: Decrease in the solid mass reservoir through pebble drift
• Collisional Growth of Icy Dust Aggregates in Disk Formation Stage: Difficulties for Planetesimal Formation via Direct Collisional Growth outside the Snowline
• Cosmic Dust Aggregation with Stochastic Charging
• The Nonlinear Ohm's Law: Plasma Heating by Strong Electric Fields and its Effects on the Ionization Balance in Protoplanetary Disks
• Inhibited Coagulation of Micron-size Dust Due to the Electrostatic Barrier
• Electron Heating in the Magnetorotational Instability: Implications for Turbulence Strength in Outer Regions of Protoplanetary Disks
• A Possible Mechanism for Overcoming the Electrostatic Barrier Against Dust Growth in Protoplanetary disks
• Observation of bottom-up formation for charged grain aggregates related to pre-planetary evolution beyond the bouncing barrier
• Grain charging in protoplanetary discs
• The impact of dust evolution on the dead zone outer edge in magnetized protoplanetary disks
• Coagulation-Fragmentation Equilibrium for Charged Dust: Abundance of Submicron Grains Increases Dramatically in Protoplanetary Disks
• Planetesimal Formation by Gravitational Instability of a Porous-Dust Disk
• Detailed Model of the Growth of Fluffy Dust Aggregates in a Protoplanetary Disk: Effects of Nebular Conditions
• Ionization chemistry in the inner disc: a combined treatment of ionic and thermionic emission and arbitrary grain size distributions
• Dust Coagulation in the Vicinity of a Gap-Opening Jupiter-Mass Planet
• Linear Analysis of the Nonaxisymmetric Secular Gravitational Instability