Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks

Abstract

The growth of solid particles towards meter sizes in protoplanetary disks has to circumvent at least two hurdles, namely the rapid loss of material due to radial drift and particle fragmentation due to destructive collisions. In this paper, we present the results of numerical simulations with more and more realistic physics involved. Step by step, we include various effects, such as particle growth, radial/vertical particle motion and dust particle fragmentation in our simulations. We demonstrate that the initial dust-to-gas ratio is essential for the particles to overcome the radial drift barrier. If this value is increased by a factor of 2 compared with the canonical value for the interstellar medium, km-sized bodies can form in the inner disk <2 AU within 10 thousand years. However, we find that solid particles get destroyed through collisional fragmentation. Only with the unrealistically high-threshold velocities needed for fragmentation to occur (>30 m/s), particles are able to grow to larger sizes in low turbulent disks. We also find that less than 5% of the small dust grains remain in the disk after 1 Myrs due to radial drift, no matter whether fragmentation is included in the simulations or not. In this paper, we also present considerable improvements to existing algorithms for dust-particle coagulation, which speed up the coagulation scheme by a factor of 10 thousand.

accepted for publication in A&A

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• A sub-grid model for the growth of dust particles in hydrodynamical simulations of protoplanetary disks
• Mass determination of protoplanetary disks from dust evolution
• The effect of the regular solution model in the condensation of protoplanetary dust
• Thermal inertias of pebble-pile comet 67P/Churyumov-Gerasimenko
• Dust Coagulation Regulated by Turbulent Clustering in Protoplanetary Disks
• The dimming of RW Auriga. Is dust accretion preceding an outburst?
• Formation of wide-orbit giant planets in protoplanetary disks with a decreasing pebble flux
• Theory of planet formation
• Dust Growth and Dynamics in Protoplanetary Nebulae: Implications for Opacity, Thermal Profile and Gravitational Instability
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
• Presolar grain dynamics: creating nucleosynthetic variations through a combination of drag and viscous evolution
• Implementation of dust particles in three-dimensional magnetohydrodynamics simulation: Dust dynamics in a collapsing cloud core
• The observational impact of dust trapping in self-gravitating discs
• AB Aurigae: Possible evidence of planet formation through the gravitational instability
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Ring Morphology with Dust Coagulation in Protoplanetary Disks
• Planetary core formation via multi-species pebble accretion
• Dust Grain Evolution in Spatially Resolved T Tauri Binaries
• 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 Spherically Symmetric Gravitational Collapse of a Clump of Solids in a Gas
• Free Collisions in a Microgravity Many-Particle Experiment. IV. - Three-Dimensional Analysis of Collision Properties
• Planet population synthesis: The role of stellar encounters
• The growth of super-Earths: the importance of a self-consistent treatment of disc structures and pebble accretion
• Collisions of solid ice in planetesimal formation
• The effect of the streaming instability on protoplanetary disc emission at millimetre wavelengths
• Analysis of Methods for Computing the Trajectories of Dust Particles in a Gas-Dust Circumstellar Disk
• Coagulation-Fragmentation Equilibrium for Charged Dust: Abundance of Submicron Grains Increases Dramatically in Protoplanetary Disks
• Global Self-Similar Protostellar Disk/Wind Models
• Imaging the disc rim and a moving close-in companion candidate in the pre-transitional disc of V1247 Orionis
• Effect of Elastic Vibrations on Normal Head on Collisions of Isothermal Spheres
• Phyllosilicate Emission from Protoplanetary Disks: Is the Indirect Detection of Extrasolar Water Possible?
• Search for substellar-mass companions and asymmetries in their parent discs
• Growing dust grains in protoplanetary discs - I. Radial drift with toy growth models
• Effect of Different Angular Momentum Transport mechanisms on the Distribution of Water in Protoplanetary Disks
• Chemical evolution in planet-forming regions with growing grains
• Millimeter emission in photoevaporating disks is determined by early substructures
• Size and density sorting of dust grains in SPH simulations of protoplanetary disc II: Fragmentation
• A slim disc approach to external photoevaporation of discs
• A quantification of hydrodynamical effects on protoplanetary dust growth
• Global Modeling of Nebulae With Particle Growth, Drift, and Evaporation Fronts. III. Redistribution of Refractories and Volatiles
• Formation of the First Planetesimals via the Streaming Instability in Globally Turbulent Protoplanetary Disks?
• ALMA observation of the protoplanetary disk around WW Cha: faint double-peaked ring and asymmetric structure
• TEMPus VoLA: the Timed Epstein Multi-pressure Vessel at Low Accelerations
• A Pluto-Charon Sonata III. Growth of Charon from a Circum-Pluto Ring of Debris
• Non-axisymmetric instabilities in discs with imposed zonal flows
• The role of density perturbation on planet formation by pebble accretion
• Constraining giant planet formation with synthetic ALMA images of the Solar System's natal protoplanetary disk
• How external photo-evaporation changes the chemical composition of the inner disc
• The solar abundance problem and eMSTOs in clusters
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Imaging the Dusty Substructures due to Terrestrial Planets in Planet-forming Disks with ALMA and the Next Generation Very Large Array
• Iceline Variations Driven by Protoplanetary Disc Gaps
• Shaping the CO snowline in protoplanetary disks
• On Secular Gravitational Instability in Vertically Stratified Disks
• Dust grain shattering in protoplanetary discs: collisional fragmentation or rotational disruption?
• Super-Earth formation in systems with cold giants
• Substructures in protoplanetary disks imprinted by compact planetary systems
• The mm-colors of a young binary disk system in the Orion Nebula Cluster
• Multi-frequency analysis of the ALMA and VLA high resolution continuum observations of the substructured disc around CI Tau. Preference for sub-mm-sized low-porosity amorphous carbon grains
• Structure of Protoplanetary Discs with Magnetically-driven Winds
• Seeing the unseen: a method to detect unresolved rings in protoplanetary disks
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I: First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
• Dynamic evolution of major element chemistry in protoplanetary disks and its implications for chondrite formation
• How Flow Isolation May Set the Mass Scale for Super-Earth Planets
• Detecting circumstellar disks around gravitational microlenses
• A formation pathway for terrestrial planets with moderate water content involving atmospheric-volatile recycling
• Jamming and Tiling in Fragmentation of Rectangles
• O(N^2) fragmentation algorithm
• Emerging population of gap-opening planets around type-A stars -- Long-term evolution of the forming planets around HD 163296
• ALMA Observations of the Inner Cavity in the Protoplanetary Disk around Sz 84
• Size-selective accretion of dust onto CPDs: Low CPD masses and filtration of larger grains
• Changing disc compositions via internal photoevaporation II: M dwarf systems
• Properties of outer solar system pebbles during planetesimal formation from meteor observations
• Emission from Magnetized Accretion Disks around Young Stars
• Ionizing Protoplanetary Disks in Pebble Collisions
• Exploring the Grain Properties in the Disk of HL Tau with an Evolutionary Model
• On the Courant-Friedrichs-Lewy condition for numerical solvers of the coagulation equation
• How does the chemical composition of solids influence the formation of planetesimals?
• How disc initial conditions sculpt the atmospheric composition of giant planets
• Impact of dust diffusion on the rim shape of protoplanetary disks
• Exploring the conditions for forming planetesimals by the streaming instability and planetary systems by pebble accretion
• Zero Age Planetary Orbit of Gas Giant Planets Revisited: Reinforcement of the Link with Stellar Metallicity
• Evolving grain-size distributions embedded in gas flows
• SHAMPOO: A stochastic model for tracking dust particles under the influence of non-local disk processes
• The Radial Profile of Dust Grain Size in the Protoplanetary Disk of DS Tau
• Planet Mass Function around M stars at 1-10 au: A Plethora of sub-Earth mass objects
• Formation of stars and planets: the role of magnetic fields
• Models and Observational Predictions of Dust Traps in Protoplanetary Discs
• Effects of Stellar X-ray Photoevaporation on Planetesimal Formation via the Streaming Instability
• Planetary population synthesis
• Mid-infrared absorption spectra and mass absorption coefficients for 23 chondrites: dependence on composition and grain size
• Structure of the Stellar Neighborhood of CQ Tau in the Presence of a Companion in an Elongated Orbit
• Hydrodynamical simulations of the vertical shear instability with dynamic dust and cooling rates in protoplanetary disks
• A fast tree algorithm for multi-component coagulation equation
• Molecules with ALMA at Planet-forming Scales (MAPS) XII: Inferring the C/O and S/H ratios in Protoplanetary Disks with Sulfur Molecules
• Effects of turbulent diffusion and back-reaction on the dust distribution around two resonant planets
• A close-encounter method for simulating the dynamics of planetesimals
• Formation of Water-rich Giant Planet Satellites at Decretion Disk Ice Lines
• The Substructures in Disks undergoing Vertical Shear Instability: II. Observational Predictions for the Dust Continuum
• Photoevaporation of protoplanetary disks by Far-UV photons arising from neighbouring massive stars: observation of proplyds and modelling
• MINDS survey of silicates in T Tauri disks: Correlation between dust and gas
• The Influence of the Fractal Dimension on Dust Evolution in Protoplanetary Disks
• The Outcome of the Protoplanetary Disk of Very Massive Stars
• Modelling the secular evolution of proto-planetary disc dust sizes -- A comparison between the viscous and magnetic wind case
• Grain Growth in Escaping Atmospheres: Implications for the Radius Inflation of Super-Puffs
• A multi-fluid approach for polydisperse pebble accretion: From particles to fluids, establishing the multifluid framework
• A break in planet occurrence near the pebble isolation mass should be observable by the Roman microlensing survey
• Delivery of complex organic molecules to the system of Jupiter