Planetesimal formation via the streaming instability with multiple grain sizes

Abstract

Kilometre-sized planetesimals form from pebbles of a range of sizes. We present the first simulations of the streaming instability that begin with a realistic, peaked size distribution, as expected from grain growth predictions. Our 3D numerical simulations directly form planetesimals via the gravitational collapse of pebble clouds. Models with multiple grain sizes show spatially distinct dust populations. The smallest grains in the size distribution do not participate in the formation of filaments or the planetesimals that are formed by the remaining 80% of the dust mass. This implies a size cutoff for pebbles incorporated into asteroids and comets. Disc observations cannot resolve this dust clumping. However, we show that clumping, combined with optical depth effects, can cause significant underestimates of the dust mass, with 20%-80% more dust being present even at moderate optical depths if the streaming instability is active.

arXiv commentAccepted to MNRAS, 16 pages, 10 figures

References in corpus (75)

• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• Athena: A New Code for Astrophysical MHD
• A simple model for the evolution of the dust population in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• A Major Asymmetric Dust Trap in a Transition Disk
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• FARGO: a fast eulerian transport algorithm for differentially rotating disks
• Ringed Substructure and a Gap at 1 AU in the Nearest Protoplanetary Disk
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments
• Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region
• The Disk Substructures at High Angular Resolution Project (DSHARP): II. Characteristics of Annular Substructures
• Protoplanetary Disk Turbulence Driven by the Streaming Instability: Non-Linear Saturation and Particle Concentration
• Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
• Observations of Protoplanetary Disk Structures
• Discovery of Small-Scale Spiral Structures in the Disk of SAO 206462 (HD 135344B): Implications for the Physical State of the Disk from Spiral Density Wave Theory
• The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
• Dynamics of Solids in the Midplane of Protoplanetary Disks: Implications for Planetesimal Formation
• The Disk Substructures at High Angular Resolution Project (DSHARP): V. Interpreting ALMA maps of protoplanetary disks in terms of a dust model
• Disks ARound TTauri Stars with Sphere (DARTTS-S) I: Sphere / IRDIS Polarimetric Imaging of 8 prominent TTauri Disks
• Spiral Density Waves in a Young 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
• Protoplanetary Disk Turbulence Driven by the Streaming Instability: Linear Evolution and Numerical Methods
• Asymmetric features in the protoplanetary disk MWC758
• Concentrating small particles in protoplanetary disks through the streaming instability
• Dust Evolution and the Formation of Planetesimals
• Planetesimal formation starts at the snow line
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Three-phase Interstellar medium in Galaxies Resolving Evolution with Star formation and Supernova feedback (TIGRESS): Algorithms, Fiducial model, and Convergence
• Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
• Shadows and spirals in the protoplanetary disk HD 100453
• Initial mass function of planetesimals formed by the streaming instability
• Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles
• Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities
• Rubble Pile Asteroids
• Particle-Gas Dynamics with Athena: Method and Convergence
• Thresholds for Particle Clumping by the Streaming Instability
• Impact Craters on Pluto and Charon Indicate a Deficit of Small Kuiper Belt Objects
• Implementation of the Shearing Box Approximation in Athena
• Resonant Drag Instabilities in protoplanetary disks: the streaming instability and new, faster-growing instabilities
• Self-induced dust traps: overcoming planet formation barriers
• Evidence for universality in the initial planetesimal mass function
• On the diversity of asymmetries in gapped protoplanetary disks
• Evidence for a massive dust-trapping vortex connected to spirals: a multi-wavelength analysis of the HD~135344B protoplanetary disk
• The solar nebula origin of (486958) Arrokoth, a primordial contact binary in the Kuiper belt
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient
• Demographics of Planetesimals Formed by the Streaming Instability
• Dust Evolution Can Produce Scattered Light Gaps in Protoplanetary Disks
• Streaming Instability for Particle-Size Distributions
• The initial conditions for planet formation: Turbulence driven by hydrodynamical instabilities in disks around young stars
• Protoplanetary Disk Rings as Sites for Planetesimal Formation
• The DSHARP Rings: Evidence of Ongoing Planetesimal Formation?
• A concentration of centimeter-sized grains in the Oph IRS 48 dust trap
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• On the Numerical Robustness of the Streaming Instability: Particle Concentration and Gas Dynamics in Protoplanetary Disks
• Streaming Instability with Multiple Dust Species: I. Favourable Conditions for the Linear Growth
• Polydisperse Streaming Instability I. Tightly coupled particles and the terminal velocity approximation
• Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multi-Wavelength ALMA Observations
• Streaming Instability with Multiple Dust Species: II. Turbulence and Dust-Gas Dynamics at Nonlinear Saturation
• Streaming Instability of Multiple Particle Species in Protoplanetary Disks
• The Streaming Instability Cannot Form Planetesimals from mm-size Grains in Pressure Bumps
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• Streaming instability of multiple particle species II -- Numerical convergence with increasing particle number
• Origin of (2014) MU69-like Kuiper-belt contact binaries from wide binaries
• Planetesimal Initial Mass Functions following Diffusion Regulated Gravitational Collapse
• Polydisperse Streaming Instability II. Methods for solving the linear stability problem
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Constraining the turbulence and the dust disk in IM Lup: onset of planetesimal formation
• Constraining the final merger of contact binary(486958) Arrokoth with soft-sphere discrete element simulations
• Streaming instability on different scales. I. Planetesimal mass distribution variability
• The effect of the streaming instability on protoplanetary disc emission at millimetre wavelengths

Cited by in corpus (4)

• Polydisperse Formation of Planetesimals: The dust size distribution in clumps
• Resonant drag instabilities for polydisperse dust. II. The streaming and settling instabilities
• Evading the dust fragmentation barrier with the streaming instability in protoplanetary disks
• Streaming instabilities in accreting protoplanetary disks: A parameter study