Prompt planetesimal formation beyond the snow line

Abstract

We develop a simple model to predict the radial distribution of planetesimal formation. The model is based on the observed growth of dust to mm-sized particles, which drift radially, pile-up, and form planetesimals where the stopping time and dust-to-gas ratio intersect the allowed region for streaming instability-induced gravitational collapse. Using an approximate analytic treatment, we first show that drifting particles define a track in metallicity--stopping time space whose only substantial dependence is on the disk's angular momentum transport efficiency. Prompt planetesimal formation is feasible for high particle accretion rates (relative to the gas, ${\dot{M}}_p/\dot{M}>3\times 10^{-2}$ for $\alpha =10^{-2}$), that could only be sustained for a limited period of time. If it is possible, it would lead to the deposition of a broad and massive belt of planetesimals with a sharp outer edge. Including turbulent diffusion and vapor condensation processes numerically, we find that a modest enhancement of solids near the snow line occurs for cm-sized particles, but that this is largely immaterial for planetesimal formation. We note that radial drift couples planetesimal formation across radii in the disk, and suggest that considerations of planetesimal formation favor a model in which the initial deposition of material for giant planet cores occurs well beyond the snow line.

arXiv commentApJ Letters, in press

References in corpus (29)

• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region
• A simple model for the evolution of the dust population in protoplanetary disks
• Planet-disk interaction and orbital evolution
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• Planetesimal Formation by Gravitational Instability
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Radial Flow of Dust Particles in Accretion Disks
• Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
• An Old Disk That Can Still Form a Planetary System
• The Evolution of the Water Distribution in a Viscous Protoplanetary Disk
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• The stickiness of micrometer-sized water-ice particles
• A Parametric Modeling Approach to Measuring the Gas Masses of Circumstellar Disks
• Fluffy dust forms icy planetesimals by static compression
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Growing the gas-giant planets by the gradual accumulation of pebbles
• Dust dynamics during protoplanetary disc clearing
• Evidence for a correlation between mass accretion rates onto young stars and the mass of their protoplanetary disks
• Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks
• Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities
• The Effect of the Radial Pressure Gradient in Protoplanetary Disks on Planetesimal Formation
• Magnetically driven accretion in protoplanetary discs
• Can dust coagulation trigger streaming instability?
• Particle Pile-ups and Planetesimal Formation
• A panoptic model for planetesimal formation and pebble delivery
• Protoplanetary Disks in the Orion OMC1 Region Imaged with ALMA
• Global variation of the dust-to-gas ratio in evolving protoplanetary discs

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• The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview
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• Planetesimal formation starts at the snow line
• Planetesimal formation near the snowline: in or out?
• Astrochemistry and compositions of planetary systems
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• The nature and origins of sub-Neptune size planets
• Resonant Drag Instabilities in protoplanetary disks: the streaming instability and new, faster-growing instabilities
• Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line
• Characterizing Exoplanet Habitability
• Origin of Earth's water: sources and constraints
• Solar System Formation in the Context of Extra-Solar Planets
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient
• Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion and disc evolution
• How efficient is the streaming instability in viscous protoplanetary disks?
• The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
• A Lagrangian Model for Dust Evolution in Protoplanetary Disks: Formation of Wet and Dry Planetesimals at Different Stellar Masses
• Formation of rocky and icy planetesimals inside and outside the snow line: Effects of diffusion, sublimation and back-reaction
• Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains
• Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain
• The water-ice line as a birthplace of planets: Implications of a species-dependent dust fragmentation threshold
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Formation of Terrestrial Planets
• Enrichment of Jupiter's atmosphere by late planetesimal bombardment
• The subsurface habitability of small, icy exomoons
• Formation of super-Earths and mini-Neptunes from rings of planetesimals
• An analysis of binary microlensing event OGLE-2015-BLG-0060
• Planet formation: key mechanisms and global models
• A "no-drift" runaway pile-up of pebbles in protoplanetary disks II. Characteristics of the resulting planetesimal belt
• Numerical Insights into Disk Accretion, Eccentricity, and Kinematics in the Class 0 phase