Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities

Abstract

Modelling the formation of super-km-sized planetesimals by gravitational collapse of regions overdense in small particles requires numerical algorithms capable of handling simultaneously hydrodynamics, particle dynamics and particle collisions. While the initial phases of radial contraction are dictated by drag forces and gravity, particle collisions become gradually more significant as filaments contract beyond Roche density. Here we present a new numerical algorithm for treating momentum and energy exchange in collisions between numerical superparticles representing a high number of physical particles. We adopt a Monte Carlo approach where superparticle pairs in a grid cell collide statistically on the physical collision time-scale. Collisions occur by enlarging particles until they touch and solving for the collision outcome, accounting for energy dissipation in inelastic collisions. We demonstrate that superparticle collisions can be consistently implemented at a modest computational cost. In protoplanetary disc turbulence driven by the streaming instability, we argue that the relative Keplerian shear velocity should be subtracted during the collision calculation. If it is not subtracted, density inhomogeneities are too rapidly diffused away, as bloated particles exaggerate collision speeds. Local particle densities reach several thousand times the mid-plane gas density. We find efficient formation of gravitationally bound clumps, with a range of masses corresponding to contracted radii from 100 to 400 km when applied to the asteroid belt and 150 to 730 km when applied to the Kuiper belt, extrapolated using a constant self-gravity parameter. The smaller planetesimals are not observed at low resolution, but the masses of the largest planetesimals are relatively independent of resolution and treatment of collisions.

Version accepted for publication in A&A

References in corpus (12)

• On the Formation of Planetesimals via Secular Gravitational Instabilities with Turbulent Stirring
• Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks
• High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• Turbulent Clustering of Protoplanetary Dust and Planetesimal Formation
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• Microgravity experiments on the collisional behavior of Saturnian ring particles
• The Gravitational instability of solids assisted by gas drag: slowing by turbulent mass diffusivity
• $N$-body Simulation of Planetesimal Formation Through Gravitational Instability of a Dust Layer
• Binary formation and mass function variations in fragmenting discs with short cooling times
• Forming Planetesimals by Gravitational Instability: II. How Dust Settles to its Marginally Stable State
• Collisional Particle Disks

Cited by in corpus (99)

• Rapid growth of gas-giant cores by pebble accretion
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Concentrating small particles in protoplanetary disks through the streaming instability
• Dust Evolution and the Formation of Planetesimals
• The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars
• Initial mass function of planetesimals formed by the streaming instability
• The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
• Thresholds for Particle Clumping by the Streaming Instability
• Resolved Debris Discs Around A Stars in the Herschel DEBRIS Survey
• Resonant Drag Instabilities in protoplanetary disks: the streaming instability and new, faster-growing instabilities
• Collisional Aggregation due to Turbulence
• Evidence for universality in the initial planetesimal mass function
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient
• Formation of pebble-pile planetesimals
• Multiple and Fast: The Accretion of Ordinary Chondrite Parent Bodies
• Protoplanetary Disk Rings as Sites for Planetesimal Formation
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• Understanding how planets become massive. I. Description and validation of a new toy model
• The formation of the solar system
• On the Feeding Zone of Planetesimal Formation by the Streaming Instability
• Pebble-driven Planet Formation around Very Low-mass Stars and Brown Dwarfs
• Herschel's "Cold Debris Disks": Background Galaxies or Quiescent Rims of Planetary Systems?
• Stirring in massive, young debris discs from spatially resolved Herschel images
• A Tale of Planet Formation: From Dust to Planets
• Growth after the streaming instability: from planetesimal accretion to pebble accretion
• On the Numerical Robustness of the Streaming Instability: Particle Concentration and Gas Dynamics in Protoplanetary Disks
• On the growth of pebble-accreting planetesimals
• Diverse protoplanetary disk morphology produced by a Jupiter-mass planet
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Dust and gas density evolution at a radial pressure bump in protoplanetary disks
• SMACK: A New Algorithm for Modeling Collisions and Dynamics of Planetesimals in Debris Disks
• The physics of protoplanetesimal dust agglomerates. VII The low-velocity collision behavior of large dust agglomerates
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• Birth Locations of the Kepler Circumbinary Planets
• Effect of dust radial drift on viscous evolution of gaseous disk
• Linear growth of streaming instability in pressure bumps
• Modeling dust growth in protoplanetary disks: The breakthrough case
• Prompt planetesimal formation beyond the snow line
• The Demographics of Rocky Free-Floating Planets and their Detectability by WFIRST
• Formation of solar system analogs I: looking for initial conditions through a population synthesis analysis
• A method for coupling dynamical and collisional evolution of dust in circumstellar disks: the effect of a dead zone
• Impacts of dust feedback on a dust ring induced by a planet in a protoplanetary disk
• The role of pebble fragmentation in planetesimal formation I. Experimental study
• Streaming Instability of Multiple Particle Species in Protoplanetary Disks
• From Disks to Planets
• Submillimetre-sized dust aggregate collision and growth properties
• Jumping the Gap: The Formation Conditions and Mass Function of Pebble-Pile Planetesimals
• Formation of Super-Earth Mass Planets at 125-250 AU from a Solar-type Star
• A $75\%$ Occurrence Rate of Debris Discs around F stars in the $\beta$ Pic Moving Group
• New Paradigms For Asteroid Formation
• Eulerian and modified Lagrangian approaches to multi-dimensional condensation and collection
• Formation of the polar debris disc around 99 Herculis
• Formation of Comets
• Some Stars are Totally Metal: A New Mechanism Driving Dust Across Star-Forming Clouds, and Consequences for Planets, Stars, and Galaxies
• Condensational and collisional growth of cloud droplets in a turbulent environment
• The role of pebble fragmentation in planetesimal formation II. Numerical simulations
• A Simple Phenomenological Model for Grain Clustering in Turbulence
• Early formation of moons around large trans-Neptunian objects via giant impacts
• From Dust to Planets I: Planetesimal and Embryo Formation
• Effect of turbulence on collisional growth of cloud droplets
• Dusty spirals triggered by shadows in transition discs
• Formation of Terrestrial Planets
• Migration processes in the Solar System and their role in the evolution of the Earth and planets
• Planetesimal formation in self-gravitating discs -- dust trapping by vortices
• Pebble accretion in class 0/I YSOs as a possible pathway for early planet formation
• Spontaneous concentrations of solids through two-way drag forces between gas and sedimenting particles
• Cloud-droplet growth due to supersaturation fluctuations in stratiform clouds
• Are there any pristine comets? Constraints from pebble structure
• New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds
• Making the Solar System
• Potential multi-component structure of the debris disk around HIP 17439 revealed by Herschel/DUNES
• Channels for streaming instability in dusty discs
• Collision fluctuations of lucky droplets with superdroplets
• Bi-lobed Shape of Comet 67P from a Collapsed Binary
• Formation of pebbles in (gravito-)viscous protoplanetary disks with various turbulent strengths
• Dust-vortex instability in the regime of well-coupled grains
• Exoplanetary Geophysics -- An Emerging Discipline
• AB Aurigae: Possible evidence of planet formation through the gravitational instability
• Streaming instability on different scales. I. Planetesimal mass distribution variability
• Planetesimal formation via the streaming instability with multiple grain sizes
• Coagulation Calculations of Icy Planet Formation Around 0.1--0.5~\msun\ Stars: Super-Earths From Large Planetestimals
• Dust-gas dynamics driven by the streaming instability with various pressure gradients
• A brief overview of planet formation
• Can the giant planets of the Solar System form via pebble accretion in a smooth protoplanetary disc?
• MRI-active inner regions of protoplanetary discs. II. Dependence on dust, disc and stellar parameters
• Formation of the Earth and Moon: Influence of Small Bodies
• Formation of trans-Neptunian satellite systems at the stage of condensations
• Formation of embryos of the Earth and the Moon from the common rarefied condensation and their subsequent growth
• Observation of aerodynamic instability in the flow of a particle stream in a dilute gas
• Origin of orbits of secondaries in the discovered trans-Neptunian binaries
• Coagulation of inertial particles in supersonic turbulence
• Aggregate Growth and Internal structures of Chondrite Parent Bodies Forming from Dense Clumps
• Delivery of icy planetesimals to inner planets in the Proxima Centauri planetary system
• Growth of the Moon due to bodies ejected from the Earth
• Angular momenta of collided rarefied preplanetesimals
• Growth of asteroids, planetary embryos and Kuiper belt objects by chondrule accretion
• Migration of celestial bodies in the Solar system and in several exoplanetary systems
• A close-encounter method for simulating the dynamics of planetesimals