Erosion and the limits to planetesimal growth

Abstract

The coagulation of microscopic dust into planetesimals is the first step towards planet formation. The size and shape of the growing aggregates determine the efficiency of this early growth. It has been proposed that fluffy ice aggregates can grow very efficiently, suffering less from the bouncing and radial drift barriers. While the collision velocity between icy aggregates of similar size is thought to stay below the fragmentation threshold, they may nonetheless lose mass from collisions with much smaller projectiles. We investigate the effect of these erosive collisions on the ability of porous ice aggregates to cross the radial drift barrier. We develop a Monte Carlo code that calculates the evolution of the growing aggregates, while resolving the entire mass distribution at all times. The aggregate's porosity is treated independently of its mass, and is determined by collisions, gas compaction, and eventually self-gravity compaction. For erosion threshold velocities of 20-40 m/s, high-velocity collisions with small projectiles prevent the largest aggregates from growing when they start to drift. In these cases, our local simulations result in a steady-state distribution, with the majority of the dust mass in particles with Stokes numbers close to unity. Only for the highest erosion threshold considered (60 m/s), do porous aggregates manage to cross the radial drift barrier in the inner 10 AU of MMSN-like disks. Erosive collisions are more effective in limiting the growth than fragmentary collisions between similar-size particles. Conceivably, erosion limits the growth before the radial drift barrier, although the robustness of this statement depends on (uncertain) material properties of icy aggregates. If erosion inhibits planetesimal formation through direct sticking, the sea of $\sim 10^9$ g, highly porous particles appears well-suited for triggering streaming instability.

arXiv comment16 pages, 14 figures, accepted for publication in A&A

References in corpus (40)

• Disk Frequencies and Lifetimes in Young Clusters
• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• Rapid growth of gas-giant cores by pebble accretion
• Dust coagulation in protoplanetary disks: a rapid depletion of small grains
• Gas- and dust evolution in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar 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
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Dynamics of Solids in the Midplane of Protoplanetary Disks: Implications for Planetesimal Formation
• Fluffy dust forms icy planetesimals by static compression
• Dust coagulation in protoplanetary disks: porosity matters
• The Effect of the Radial Pressure Gradient in Protoplanetary Disks on Planetesimal Formation
• Numerical Modeling of the Coagulation and Porosity Evolution of Dust Aggregates
• Micrometer-sized ice particles for planetary-science experiments - I. Preparation, critical rolling friction force, and specific surface energy
• Breaking through: The effects of a velocity distribution on barriers to dust growth
• Can dust coagulation trigger streaming instability?
• Opacity of fluffy dust aggregates
• From dust to planetesimals: an improved model for collisional growth in protoplanetary disks
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• 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
• Static compression of porous dust aggregates
• Geometrical Cross Sections of Dust Aggregates and a Compression Model for Aggregate Collisions
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Utilitarian Opacity Model for Aggregate Particles in Protoplanetary Nebulae and Exoplanet Atmospheres
• Bouncing Behavior of Microscopic Dust Aggregates
• The Physics of Protoplanetesimal Dust Agglomerates. Vi. Erosion of Large Aggregates as a Source of Micrometer-Sized Particles
• Erosion of dust aggregates
• The Physics of Protoplanetesimal Dust Agglomerates. V. Multiple Impacts of Dusty Agglomerates at Velocities Above the Fragmentation Threshold
• Challenges in Forming the Solar System's Giant Planet Cores via Pebble Accretion
• Modeling dust growth in protoplanetary disks: The breakthrough case
• Experiments on centimeter-sized dust aggregates and their implications for planetesimal formation
• Effect of dust grain porosity on the appearance of protoplanetary disks
• Coagulation of small grains in disks: the influence of residual infall and initial small-grain content
• Numerical determination of the material properties of porous dust cakes

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