The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? I. Mapping the zoo of laboratory collision experiments

Abstract

The growth processes from protoplanetary dust to planetesimals are not fully understood. Laboratory experiments and theoretical models have shown that collisions among the dust aggregates can lead to sticking, bouncing, and fragmentation. However, no systematic study on the collisional outcome of protoplanetary dust has been performed so far so that a physical model of the dust evolution in protoplanetary disks is still missing. We intend to map the parameter space for the collisional interaction of arbitrarily porous dust aggregates. This parameter space encompasses the dust-aggregate masses, their porosities and the collision velocity. With such a complete mapping of the collisional outcomes of protoplanetary dust aggregates, it will be possible to follow the collisional evolution of dust in a protoplanetary disk environment. We use literature data, perform own laboratory experiments, and apply simple physical models to get a complete picture of the collisional interaction of protoplanetary dust aggregates. In our study, we found four different types of sticking, two types of bouncing, and three types of fragmentation as possible outcomes in collisions among protoplanetary dust aggregates. We distinguish between eight combinations of porosity and mass ratio. For each of these cases, we present a complete collision model for dust-aggregate masses between 10^-12 and 10^2 g and collision velocities in the range 10^-4 to 10^4 cm/s for arbitrary porosities. This model comprises the collisional outcome, the mass(es) of the resulting aggregate(s) and their porosities. We present the first complete collision model for protoplanetary dust. This collision model can be used for the determination of the dust-growth rate in protoplanetary disks.

accepted by Astronomy and Astrophysics

References in corpus (9)

• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? II. Introducing the bouncing barrier
• Dust coagulation in protoplanetary disks: porosity matters
• High Velocity Dust Collisions: Forming Planetesimals in a Fragmentation Cascade with Final Accretion
• A representative particle approach to coagulation and fragmentation of dust aggregates and fluid droplets
• The Physics of Protoplanetesimal Dust Agglomerates. IV. Towards a Dynamical Collision Model
• The Physics of Protoplanetesimal Dust Agglomerates II. Low Velocity Collision Properties
• Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime
• Decimetre dust aggregates in protoplanetary discs
• Exposing metal and silicate charges to electrical discharges: Did chondrules form by nebular lightning?

Cited by in corpus (317)

• A simple model for the evolution of the dust population in protoplanetary disks
• Gas- and dust evolution in protoplanetary disks
• Our astrochemical heritage
• Ring shaped dust accumulation in transition disks
• Forming Planetesimals in Solar and Extrasolar Nebulae
• Observations of Protoplanetary Disk Structures
• Dynamics of Solids in the Midplane of Protoplanetary Disks: Implications for Planetesimal Formation
• Trapping dust particles in the outer regions of protoplanetary disks
• The Disk Substructures at High Angular Resolution Project (DSHARP): V. Interpreting ALMA maps of protoplanetary disks in terms of a dust model
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• The nature of the TRAPPIST-1 exoplanets
• The stickiness of micrometer-sized water-ice particles
• Pebble isolation mass --- scaling law and implications for the formation of super-Earths and gas giants
• Dust Evolution and the Formation of Planetesimals
• Molecules with ALMA at Planet-forming Scales (MAPS) I: Program Overview and Highlights
• Planetesimal formation starts at the snow line
• Fluffy dust forms icy planetesimals by static compression
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Astrochemistry and compositions of planetary systems
• Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
• Close-in planetesimal formation by pile-up of drifting pebbles
• Dust release and tensile strength of the non-volatile layer of cometary nuclei
• Free Collisions in a Microgravity Many-Particle Experiment. I. Dust Aggregate Sticking at Low Velocities
• 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
• Growing the terrestrial planets from the gradual accumulation of sub-meter sized objects
• The Radial Distribution of Dust Particles in the HL Tau Disk from ALMA and VLA Observations
• The Effect of the Radial Pressure Gradient in Protoplanetary Disks on Planetesimal Formation
• How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
• Formation of TRAPPIST-1 and other compact systems
• Micrometer-sized ice particles for planetary-science experiments - I. Preparation, critical rolling friction force, and specific surface energy
• The Impact of Dust Evolution and Photoevaporation on Disk Dispersal
• Planetesimal formation by the streaming instability in a photoevaporating disk
• Breaking through: The effects of a velocity distribution on barriers to dust growth
• High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
• Can dust coagulation trigger streaming instability?
• Size distribution of particles in Saturn's rings from aggregation and fragmentation
• Dust evolution in protoplanetary discs and the formation of planetesimals. What have we learned from laboratory experiments?
• Contemporary formation of early solar system planetesimals at two distinct radial locations
• Global Models of Planet Formation and Evolution
• Transport of CO in Protoplanetary Disks: Consequences of Pebble Formation, Settling, and Radial Drift
• Towards a Population Synthesis Model of Objects formed by Self-Gravitating Disc Fragmentation and Tidal Downsizing
• Can grain growth explain transition disks?
• Testing the theory of grain growth and fragmentation by millimeter observations of protoplanetary disks
• From dust to planetesimals: an improved model for collisional growth in protoplanetary disks
• Dust growth and evolution in protoplanetary disks
• Comets formed in solar-nebula instabilities! -- An experimental and modeling attempt to relate the activity of comets to their formation process (corrigendum included)
• Super-Earth masses sculpted by pebble isolation around stars of different masses
• Cohesion of Amorphous Silica Spheres: Toward a Better Understanding of the Coagulation Growth of Silicate Dust Aggregates
• Low-velocity collisions of centimeter-sized dust aggregates
• Particle Trapping and Streaming Instability in Vortices
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient
• Grain opacity and the bulk composition of extrasolar planets. II. An analytical model for the grain opacity in protoplanetary atmospheres
• Erosion and the limits to planetesimal growth
• Formation of pebble-pile planetesimals
• Turbulent Clustering of Protoplanetary Dust and Planetesimal Formation
• Catching drifting pebbles I. Enhanced pebble accretion efficiencies for eccentric planets
• Dust Evolution Can Produce Scattered Light Gaps in Protoplanetary Disks
• Thermal conductivity measurements of porous dust aggregates: I. Technique, model and first results
• The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? III. Sedimentation driven coagulation inside the snow-line
• Electrostatic Barrier against Dust Growth in Protoplanetary Disks. I. Classifying the Evolution of Size Distribution
• Tracing water vapor and ice during dust growth
• Atmospheres of Brown Dwarfs
• Protoplanetary Disk Rings as Sites for Planetesimal Formation
• A panoptic model for planetesimal formation and pebble delivery
• Redistribution of CO at the Location of the CO Ice Line in evolving Gas and Dust Disks
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• Explaining millimeter-sized particles in brown dwarf disks
• Streaming Instability in Turbulent Protoplanetary Disks
• Collisions of CO${}_2$ Ice Grains in Planet Formation
• Understanding how planets become massive. I. Description and validation of a new toy model
• The formation of the solar system
• Free Collisions in a Microgravity Many-Particle Experiment III: The Collision Behavior of sub-Millimeter-Sized Dust Aggregates
• Pebble-driven Planet Formation around Very Low-mass Stars and Brown Dwarfs
• Geometrical Cross Sections of Dust Aggregates and a Compression Model for Aggregate Collisions
• Herschel's "Cold Debris Disks": Background Galaxies or Quiescent Rims of Planetary Systems?
• Dust-driven viscous ring-instability in protoplanetary disks
• Accretion among preplanetary bodies: the many faces of runaway growth
• Planetary Core Formation with Collisional Fragmentation and Atmosphere to Form Gas Giant Planets
• Planetesimal formation via sweep-up growth at the inner edge of dead zones
• Turbulence-Induced Relative Velocity of Dust Particles I: Identical Particles
• Pebble Accretion and the Diversity of Planetary Systems
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• Electrostatic Barrier against Dust Growth in Protoplanetary Disks. II. Measuring the Size of the "Frozen" Zone
• Global Modeling of Nebulae with Particle Growth, Drift and Evaporation Fronts. I: Methodology and Typical Results
• Utilitarian Opacity Model for Aggregate Particles in Protoplanetary Nebulae and Exoplanet Atmospheres
• A Tale of Planet Formation: From Dust to Planets
• How planets grow by pebble accretion. III. Emergence of an interior composition gradient
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• Growth after the streaming instability: from planetesimal accretion to pebble accretion
• The consequences of planetary migration on the minor bodies of the early Solar System
• Impact of grain evolution on the chemical structure of protoplanetary disks
• Bouncing Behavior of Microscopic Dust Aggregates
• On the growth of pebble-accreting planetesimals
• The Physics of Protoplanetesimal Dust Agglomerates. Vi. Erosion of Large Aggregates as a Source of Micrometer-Sized Particles
• Water transport in protoplanetary disks and the hydrogen isotopic composition of chondrites
• Erosion of dust aggregates
• Porosities of Protoplanetary Dust Agglomerates from Collision Experiments
• On the coexistence of the streaming instability and the vertical shear instability in protoplanetary disks
• Dust growth in protoplanetary disks - a comprehensive experimental/theoretical approach
• Collision velocity of dust grains in self-gravitating protoplanetary discs
• The Physics of Protoplanetesimal Dust Agglomerates. V. Multiple Impacts of Dusty Agglomerates at Velocities Above the Fragmentation Threshold
• Planetesimal Formation in Magnetorotationally Dead Zones: Critical Dependence on the Net Vertical Magnetic Flux
• The physics of protoplanetesimal dust agglomerates. VII The low-velocity collision behavior of large dust agglomerates
• Effect of nucleation on icy pebble growth in protoplanetary discs
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• Comet formation in collapsing pebble clouds. What cometary bulk density implies for the cloud mass and dust-to-ice ratio
• Ionisation in atmospheres of Brown Dwarfs and extrasolar planets III. Breakdown conditions for mineral clouds
• Growth and fragmentation of centimetre-sized dust aggregates: the dependence on aggregate size and porosity
• Protostellar collapse simulations in spherical geometry with dust coagulation and fragmentation
• From grains to pebbles: the influence of size distribution and chemical composition on dust emission properties
• Subsolar Al/Si and Mg/Si ratios of non-carbonaceous chondrites reveal planetesimal formation during early condensation in the protoplanetary disk
• Linear growth of streaming instability in pressure bumps
• Modeling dust growth in protoplanetary disks: The breakthrough case
• Characterization of Ring Substructures in the Protoplanetary Disk of HD 169142 from Multi-Wavelength ALMA Observations
• Self-Stirring of Debris Discs by Planetesimals Formed by Pebble Concentration
• Macroscopic Dust in Protoplanetary Disks - From Growth to Destruction
• Ionisation in atmospheres of Brown Dwarfs and extrasolar planets II Dust-induced collisional ionization
• Nucleation and growth of iron pebbles explains the formation of iron-rich planets akin to Mercury
• The role of pebble fragmentation in planetesimal formation I. Experimental study
• Dust diffusion and settling in the presence of collisions: Trapping (sub)micron grains in the midplane
• Pebble trapping in vortices: three-dimensional simulations
• Streaming Instability of Multiple Particle Species in Protoplanetary Disks
• The Streaming Instability Cannot Form Planetesimals from mm-size Grains in Pressure Bumps
• Planet Formation: An Optimized Population-Synthesis Approach
• Submillimetre-sized dust aggregate collision and growth properties
• Smoothed particle hydrodynamics simulations of gas and dust mixtures
• Turbulence-Induced Relative Velocity of Dust particles IV: the Collision Kernel
• Porous Dust Particles in Protoplanetary Disks: Application to the HL Tau Disk
• Free Collisions in a Microgravity Many-Particle Experiment. II. The Collision Dynamics of Dust-Coated Chondrules
• Millimeter-sized grains in the protostellar envelopes: where do they come from?
• Interdependence of Electric Discharge and The Magnetorotational Instability in Protoplanetary Disks
• New Paradigms For Asteroid Formation
• Trapping of giant-planet cores - I. Vortex aided trapping at the outer dead zone edge
• A large population study of protoplanetary disks: Explaining the millimeter size-luminosity relation with or without sub-structure
• Trace element geochemistry of CR chondrite metal
• Dust Settling and Clumping in MRI Turbulent Outer Protoplanetary Disks
• Collisional Growth and Fragmentation of Dust Aggregates with Low Mass Ratios. I: Critical Collision Velocity for Water Ice
• The first stages of planet formation in binary systems: How far can dust coagulation proceed?
• Influence of grain growth on the thermal structure of protoplanetary discs
• Colliding Decimetre Dust
• The quasi-universality of chondrule size as a constraint for chondrule formation models
• Planet formation via pebble accretion in externally photoevaporating discs
• Collisions of inhomogeneous pre-planetesimals
• Setting the Stage: Planet formation and Volatile Delivery
• Pebble drift and planetesimal formation in protoplanetary discs with embedded planets
• Polydisperse Streaming Instability III. Dust evolution encourages fast instability
• Accretion in Protoplanetary Disks by Collisional Fusion
• The Preservation of Super Earths and the Emergence of Gas Giants after Their Progenitor Cores have Entered the Pebble Isolation Phase
• The β Pictoris disk imaged by Herschel PACS and SPIRE
• Compression Behaviour of Porous Dust Agglomerates
• Dust evolution and satellitesimal formation in circumplanetary disks
• Rapid Formation of Jupiter and Wide-Orbit Exoplanets in Disks with Pressure Bumps
• How to make giant planets via pebble accretion
• Formation of Comets
• Streaming instability of multiple particle species II -- Numerical convergence with increasing particle number
• Numerical Simulations of Highly Porous Dust Aggregates in the Low-Velocity Collision Regime
• What pebbles are made of: Interpretation of the V883 Ori disk
• Crossing barriers in planetesimal formation: The growth of mm-dust aggregates with large constituent grains
• Ice aggregate contacts at the nm-scale
• Planetesimal formation in self-gravitating discs: the effects of particle self-gravity and back-reaction
• Gas accretion damped by dust back-reaction at the snow line
• The role of pebble fragmentation in planetesimal formation II. Numerical simulations
• Dust clearing by radial drift in evolving protoplanetary discs
• Diversity in the outcome of dust radial drift in protoplanetary discs
• Is There a Temperature Limit in Planet Formation at 1000 K?
• Collisional evolution of dust and water ice in protoplanetary discs during and after an accretion outburst
• Size Dependence of the Bouncing Barrier in Protoplanetary Dust Growth
• Collisions of small ice particles under microgravity conditions
• Turbulence-Induced Relative Velocity of Dust Particles II: The Bidisperse Case
• Global variation of the dust-to-gas ratio in evolving protoplanetary discs
• An Analytical Theory for the Growth from Planetesimals to Planets by Polydisperse Pebble Accretion
• Survival of ALMA Rings in the Absence of Pressure Maxima
• The physics of protoplanetesimal dust agglomerates. X. High-velocity collisions between small and large dust agglomerates as growth barrier
• The Christiansen Effect in Saturn's narrow dusty rings and the spectral identification of clumps in the F ring
• How planets grow by pebble accretion IV: Envelope opacity trends from sedimenting dust and pebbles
• The aeolian-erosion barrier for the growth of metre-size objects in protoplanetary-discs
• Composition and Size Dependent Sorting in Preplanetary Growth: Seeding the Formation of Mercury-like Planets
• Growing into and out of the bouncing barrier in planetesimal formation
• Rocky Planetesimal Formation Aided by Organics
• The water-ice line as a birthplace of planets: Implications of a species-dependent dust fragmentation threshold
• The four-populations model: a new classification scheme for pre-planetesimal collisions
• Self-Induced Dust Traps Around Snow Lines in Protoplanetary Discs
• Investigating Gravitational Collapse of a Pebble Cloud to form Transneptunian Binaries
• Formation of Terrestrial Planets
• Turbulence Induced Collision Velocities and Rates between Different Sized Dust Grains
• Learning about comets from the study of mass distributions and fluxes of meteoroid streams
• Radially resolved simulations of collapsing pebble clouds in protoplanetary discs
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• A Smoking Gun for Planetesimal Formation: Charge Driven Growth into a New Size Range
• The Physics of Protoplanetesimal Dust Agglomerates. X. Mechanical properties of dust aggregates probed by a solid-projectile impact
• An inflationary disk phase to explain extended protoplanetary dust disks
• Spherical Ornstein-Uhlenbeck processes
• Tracking Dust Grains During Transport and Growth in Protoplanetary Disks
• Turbulence induced collisional velocities and density enhancements: large inertial range results from shell models
• Evidence for Pebbles in Comets
• Are Pebble Pile Planetesimals Doomed?
• The footprint of cometary dust analogs: I. Laboratory experiments of low-velocity impacts and comparison with Rosetta data
• Making the Solar System
• Collisional Growth and Fragmentation of Dust Aggregates. II. Mass Distribution of Icy Fragments
• Turbulence-Induced Relative Velocity of Dust Particles III: The Probability Distribution
• Low-velocity collision behaviour of clusters composed of sub-mm sized dust aggregates
• Chondrule destruction in nebular shocks
• Growth of Aggregates with Liquid-Like Ice-Shells in Protoplanetary Discs
• Global N-body simulations of circumbinary planet formation around Kepler-16 and -34 analogues I: Exploring the pebble accretion scenario
• Explaining Mercury's Density through Magnetic Erosion
• Pebble-driven migration of low-mass planets in the 2D regime of pebble accretion
• Mineral Snowflakes on Exoplanets and Brown Dwarfs: Coagulation and Fragmentation of Cloud Particles with {\sc HyLandS}
• Observation of bottom-up formation for charged grain aggregates related to pre-planetary evolution beyond the bouncing barrier
• Thermal processing of primordial pebbles in evolving protoplanetary disks
• Breakthrough revisited: investigating the requirements for growth of dust beyond the bouncing barrier
• Compound Chondrules fused Cold
• The Roles of Dust Growth in the Temperature Evolution and Snow Line Migration in Magnetically Accreting Protoplanetary Disks
• Compaction during fragmentation and bouncing produces realistic dust grain porosities in protoplanetary discs
• Growing the seeds of pebble accretion through planetesimal accretion
• Primordial Dusty Rings and Episodic Outbursts in Protoplanetary Discs
• Planetesimal Formation at the Boundary Between Steady Super/Sub-Keplerian Flow Created by Inhomogeneous Growth of Magnetorotational Instability
• Mass determination of protoplanetary disks from dust evolution
• A sub-grid model for the growth of dust particles in hydrodynamical simulations of protoplanetary disks
• CAI formation in the early Solar System
• Ionisation and discharge in cloud-forming atmospheres of brown dwarfs and extrasolar planets
• Dust Growth and Dynamics in Protoplanetary Nebulae: Implications for Opacity, Thermal Profile and Gravitational Instability
• The growth of super-large pre-planetary pebbles to an impact erosion limit
• Turbulent Thermal Diffusion: A Way to Concentrate Dust in Protoplanetary Discs
• Thermal inertias of pebble-pile comet 67P/Churyumov-Gerasimenko
• The dimming of RW Auriga. Is dust accretion preceding an outburst?
• Limits on Protoplanet Growth by Accretion of Small Solids
• Dust Coagulation Regulated by Turbulent Clustering in Protoplanetary Disks
• Formation of wide-orbit giant planets in protoplanetary disks with a decreasing pebble flux
• The initial structure of chondrule dust rims I: electrically neutral grains
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
• Accretion of dust by chondrules in a MHD-turbulent solar nebula
• The observational impact of dust trapping in self-gravitating discs
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Free Collisions in a Microgravity Many-Particle Experiment. IV. - Three-Dimensional Analysis of Collision Properties
• Impacts of viscous dissipation on collisional growth and fragmentation of dust aggregates
• Growth after the streaming instability: The radial distance dependence of the planetary growth
• The Effects of Protostellar Disk Turbulence on CO Emission Lines: A Comparison Study of Disks with Constant CO Abundance vs. Chemically Evolving Disks
• A Statistical Model of Aggregates Fragmentation
• The Suborbital Particle Aggregation and Collision Experiment (SPACE): Studying the Collision Behavior of Submillimeter-Sized Dust Aggregates on the Suborbital Rocket Flight REXUS 12
• Planetesimal formation via the streaming instability with multiple grain sizes
• Dust-Gas Coupling in Turbulence- and MHD Wind-Driven Protoplanetary Disks: Implications for Rocky Planet Formation
• Non-extensive super-cluster states in aggregation with fragmentation
• Transport, destruction and growth of pebbles in the gas envelope of a protoplanet
• A brief overview of planet formation
• Can the giant planets of the Solar System form via pebble accretion in a smooth protoplanetary disc?
• Making Terrestrial Planets: High Temperatures, FU Orionis Outbursts, Earth, and Planetary System Architectures
• Below One Earth Mass: The Detection, Formation, and Properties of Subterrestrial Worlds
• Positive Feedback: How a Synergy Between the Streaming Instability and Dust Coagulation Forms Planetesimals
• Onset of planet formation in the warm inner disk -- Colliding dust aggregates at high temperatures
• The cosmochemistry of planetary systems
• Fine-grained rim formation -- high speed, kinetic dust aggregation in the early Solar System
• Nano-grain depletion in photon-dominated regions
• Erosion of planetesimals by gas flow
• Sub-mm/mm optical properties of real protoplanetary matter derived from Rosetta/MIRO observations of comet 67P
• Fast formation of large ice pebbles after FU Orionis outbursts
• Refractory carbon depletion by photolysis through dust collisions and vertical mixing
• Threshold velocity for collisional growth of porous dust aggregates consisting of cohesive frictionless spheres
• Ferromagnetism and particle collisions: applications to protoplanetary disks and the meteoritical record
• Migration traps as the root cause of the Kepler dichotomy
• A quantification of hydrodynamical effects on protoplanetary dust growth
• A method to distinguish between micro- and macro-granular surfaces of small Solar System bodies
• Formation of the First Planetesimals via the Streaming Instability in Globally Turbulent Protoplanetary Disks?
• Massive Protostellar Disks as a Hot Laboratory of Silicate Grain Evolution
• Size and density sorting of dust grains in SPH simulations of protoplanetary disc II: Fragmentation
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. III. Redistribution of Refractories and Volatiles
• Investigating the Bouncing Barrier with Collision Simulations of Compressed Dust Aggregates
• How external photo-evaporation changes the chemical composition of the inner disc
• Multi-Particle Collisions in Microgravity: Coefficient of Restitution and Sticking Threshold for Systems of Mm-Sized Particles
• Observation of aerodynamic instability in the flow of a particle stream in a dilute gas
• On the interaction of pebble accreting embryos with the gaseous disc: importance of thermal forces
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Semarkona: Lessons for chondrule and chondrite formation
• Clouds in Exoplanetary Atmospheres
• Dust grain shattering in protoplanetary discs: collisional fragmentation or rotational disruption?
• Formation of super-Earths and mini-Neptunes from rings of planetesimals
• Collision fragmentation of aggregates. The role of the interaction potential between comprising particles
• Super-Earth formation in systems with cold giants
• Selective Aggregation Experiments on Planetesimal Formation and Mercury-Like Planets
• The motion of chondrules and other particles in a protoplanetary disc with temperature fluctuations
• O(N^2) fragmentation algorithm
• The footprint of cometary dust analogues: II. Morphology as a tracer of tensile strength and application to dust collection by the Rosetta spacecraft
• From Planetesimals to Dwarf Planets by Pebble Accretion
• Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks $\mathrm{II}$. Time-dependent model
• Collisions of small ice particles under microgravity conditions (II): Does the chemical composition of the ice change the collisional properties?
• Supercluster states and phase transitions in aggregation-fragmentation processes
• Pebble accretion in self-gravitating protostellar discs
• On the elastoplastic behavior in collisional compression of spherical dust aggregates
• Ionizing Protoplanetary Disks in Pebble Collisions
• Revisiting sticking property of submillimetre-sized aggregates
• Dust concentration and chondrule formation
• Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
• SHAMPOO: A stochastic model for tracking dust particles under the influence of non-local disk processes
• Dust growth in molecular cloud envelopes: a numerical approach
• Packing fraction of clusters formed in free-falling granular streams based on flash X-ray radiography
• Dust dynamics in RAMSES -- II. Equilibrium drift velocity distributions of charged dust grains
• Rossby wave instability in weakly ionized protoplanetary disks. II. radial B-fields
• Effects of Stellar X-ray Photoevaporation on Planetesimal Formation via the Streaming Instability
• Origin of compact exoplanetary systems during disk infall
• Dust photophoretic transport around a T Tauri star: Implications for comets composition
• The Impact of Silicate Grain Coagulation on Millimeter Emission from Massive Protostellar Disks
• Callisto's Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
• Positive Feedback II: How Dust Coagulation inside Vortices Can Form Planetesimals at Low Metallicity
• Gelation in input-driven aggregation
• Diversity in planetary architectures from pebble accretion: Water delivery to the habitable zone with pebble snow
• Thermally driven spontaneous dust accumulation in the inner regions of protoplanetary disks
• Dust Growth in ALMA Rings: II. Dusty Rossby Wave Instability
• A fast tree algorithm for multi-component coagulation equation
• Considering contact forces during the formation of planetesimals by gravitational collapse: mutual orbits, spin states, and shapes
• Rapid Formation of Super-Earths Around Low-Mass Stars
• Grain Growth in Escaping Atmospheres: Implications for the Radius Inflation of Super-Puffs
• Caustics of finitely dense inertial particles
• Formation of Water-rich Giant Planet Satellites at Decretion Disk Ice Lines
• The Influence of the Fractal Dimension on Dust Evolution in Protoplanetary Disks
• Setting the Stage: The Early History of the Solar System
• A close-encounter method for simulating the dynamics of planetesimals