Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation

Abstract

We propose an expression for a local planetesimal formation rate proportional to the instantaneous radial pebble flux. The result --- a radial planetesimal distribution --- can be used as initial condition to study the formation of planetary embryos. We follow the idea that one needs particle traps to locally enhance the dust-to-gas ratio sufficiently such that particle gas interactions can no longer prevent planetesimal formation on small scales. The location of these traps can emerge everywhere in the disk. Their occurrence and lifetime is subject of ongoing research, thus they are implemented via free parameters. This enables us to study the influence of the disk properties on the formation of planetesimals, predicting their time dependent formation rates and location of primary pebble accretion. We show that large $\alpha$-values of $0.01$ (strong turbulence) prevent the formation of planetesimals in the inner part of the disk, arguing for lower values of around $0.001$ (moderate turbulence), at which planetesimals form quickly at all places where they are needed for proto-planets. Planetesimals form as soon as dust has grown to pebbles ($\sim \mathrm{mm}$ to $\mathrm{dm}$) and the pebble flux reaches a critical value, which is after a few thousand years at $2-3$AU and after a few hundred thousand years at $20-30$AU. Planetesimal formation lasts until the pebble supply has decreased below a critical value. The final spatial planetesimal distribution is steeper compared to the initial dust and gas distribution which helps to explain the discrepancy between the minimum mass solar nebula and viscous accretion disks.

References in corpus (84)

• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks
• Rapid planetesimal formation in turbulent circumstellar discs
• Streaming Instabilities in Protoplanetary Disks
• The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview
• A simple model for the evolution of the dust population in protoplanetary disks
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• 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
• Density of asteroids
• 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
• Asteroids Were Born Big
• Planetesimal Formation by Gravitational Instability
• 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
• Closed-form expressions for particle relative velocities induced by turbulence
• Radial Flow of Dust Particles in Accretion Disks
• Linear and nonlinear evolution of the vertical shear instability in accretion discs
• Turbulence in Accretion Disks. Vorticity Generation and Angular Momentum Transport via the Global Baroclinic Instability
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Particle Clumping and Planetesimal Formation Depend Strongly on Metallicity
• Protoplanetary Disk Structures in Ophiuchus II: Extension to Fainter Sources
• The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
• Towards planetesimals: dense chondrule clumps in the protoplanetary nebula
• Dynamics of Solids in the Midplane of Protoplanetary Disks: Implications for Planetesimal Formation
• Size-selective concentration of chondrules and other small particles in protoplanetary nebula turbulence
• 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
• On the theory of disc photoevaporation
• Concentrating small particles in protoplanetary disks through the streaming instability
• Dust Evolution and the Formation of Planetesimals
• 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
• Global simulations of protoplanetary disks with net magnetic flux: I. Non-ideal MHD case
• Electric charging of dust aggregates and its effect on dust coagulation in protoplanetary disks
• Close-in planetesimal formation by pile-up of drifting pebbles
• Dust Growth and Settling in Protoplanetary Disks and Disk Spectral Energy Distributions. I. Laminar Disks
• Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles
• The subcritical baroclinic instability in local accretion disc models
• The thermal structure and the location of the snow line in the protosolar nebula: axisymmetric models with full 3-D radiative transfer
• Adding particle collisions to the formation of asteroids and Kuiper belt objects via streaming instabilities
• Population and Size Distribution of Small Jovian Trojan Asteroids
• Planetesimal formation around the snow line in MRI-driven turbulent protoplanetary disks
• Full Numerical Simulations of Catastrophic Small Body Collisions
• Convective Overstability in radially stratified accretion disks under thermal relaxation
• Planetesimal formation by the streaming instability in a photoevaporating disk
• Dust sedimentation and self-sustained Kelvin-Helmholtz turbulence in protoplanetary disk mid-planes. I. Radially symmetric simulations
• Breaking through: The effects of a velocity distribution on barriers to dust growth
• High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
• Resonant Drag Instabilities in protoplanetary disks: the streaming instability and new, faster-growing instabilities
• Vertical shear instability in accretion disc models with radiation transport
• Magnetic Flux Concentration and Zonal Flows in Magnetorotational Instability Turbulence
• Gravoturbulent Planetesimal Formation: The Positive Effect of long-lived Zonal Flows
• Formation of Giant Planets by Concurrent Accretion of Solids and Gas inside an Anti-Cyclonic Vortex
• Baroclinic Vorticity Production in Protoplanetary Disks; Part I: Vortex Formation
• Effects of dust feedback on vortices in protoplanetary disks
• The Size Distribution of Kuiper belt objects for D> 10 km
• Low-velocity collisions of centimeter-sized dust aggregates
• Convective overstability in accretion disks: 3D linear analysis and nonlinear saturation
• Particle Trapping and Streaming Instability in Vortices
• The baroclinic instability in the context of layered accretion. Self-sustained vortices and their magnetic stability in local compressible unstratified models of protoplanetary disks
• Erosion and the limits to planetesimal growth
• Baroclinic Vorticity Production in Protoplanetary Disks; Part II: Vortex Growth and Longevity
• Particle dynamics in discs with turbulence generated by the vertical shear instability
• Diffusion and Concentration of Solids in the Dead Zone of a Protoplanetary Disk
• On the vertical-shear instability in astrophysical discs
• Tracing water vapor and ice during dust growth
• 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
• A Parameter Study for Baroclinic Vortex Amplification
• Mapping the Conditions for Hydrodynamic Instability on Steady State Accretion Models of Protoplanetary Disks
• Resonant drag instability of grains streaming in fluids
• Planetesimal formation via sweep-up growth at the inner edge of dead zones
• Global Modeling of Nebulae with Particle Growth, Drift and Evaporation Fronts. I: Methodology and Typical Results
• Vortex Formation and Survival in Protoplanetary Disks subject to Vertical Shear Instability
• Vortices and the saturation of the vertical shear instability in protoplanetary disks
• The Size Distribution of the Neptune Trojans and the Missing Intermediate Sized Planetesimals
• Modeling dust growth in protoplanetary disks: The breakthrough case
• Azimuthal and Vertical Streaming Instability at High Dust-to-gas Ratios and on the Scales of Planetesimal Formation
• Linear growth of streaming instability in pressure bumps
• From Planetesimals to Planets in Turbulent Protoplanetary Disks I. Onset of Runaway Growth

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• The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• The New Generation Planetary Population Synthesis (NGPPS). I. Bern global model of planet formation and evolution, model tests, and emerging planetary systems
• How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
• CO Depletion in Protoplanetary Disks: A Unified Picture Combining Physical Sequestration and Chemical Processing
• The New Generation Planetary Population Synthesis (NGPPS). II. Planetary population of solar-like stars and overview of statistical results
• A giant exoplanet orbiting a very low-mass star challenges planet formation models
• Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization
• Planetesimal rings as the cause of the Solar System's planetary architecture
• The evolution of dust-disk sizes from a homogeneous analysis of 1-10 Myr-old stars
• Super-Earth masses sculpted by pebble isolation around stars of different masses
• Turbulence sets the length scale for planetesimal formation: Local 2D simulations of streaming instability and planetesimal formation
• The solar nebula origin of (486958) Arrokoth, a primordial contact binary in the Kuiper belt
• Protoplanetary Disk Rings as Sites for Planetesimal Formation
• Pebble-driven Planet Formation around Very Low-mass Stars and Brown Dwarfs
• RV-detected planets around M dwarfs: Challenges for core accretion models
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Giant planet formation at the pressure maxima of protoplanetary disks II. A hybrid accretion scenario
• A fading radius valley towards M-dwarfs, a persistent density valley across stellar types
• The New Generation Planetary Population Synthesis (NGPPS). V. Predetermination of planet types in global core accretion models
• The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
• Testing the Jeans, Toomre and Bonnor-Ebert concepts for planetesimal formation: 3D streaming instability simulations of diffusion regulated formation of planetesimals
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• Most super-Earths formed by dry pebble accretion are less massive than 5 Earth masses
• Pebbles versus planetesimals: the outcomes of population synthesis models
• High Resolution Parameter Study of the Vertical Shear Instability
• The impact of pebble flux regulated planetesimal formation on giant planet formation
• Exploring the conditions for forming cold gas giants through planetesimal accretion
• Planet formation via pebble accretion in externally photoevaporating discs
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• The effect of a strong pressure bump in the Sun's natal disk: Terrestrial planet formation via planetesimal accretion rather than pebble accretion
• Constraining planetesimal stirring: how sharp are debris disc edges?
• Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles
• Enriching inner discs and giant planets with heavy elements
• The coexistence of the streaming instability and the vertical shear instability in protoplanetary disks: Planetesimal formation thresholds explored in two-dimensional global models
• Composition of giant planets: the roles of pebbles and planetesimals
• Constraining the parameter space for the Solar Nebula
• The importance of thermal torques on the migration of planets growing by pebble accretion
• Early planet formation in embedded protostellar disks: Setting the stage for the first generation of planetesimals
• Linking planetary embryo formation to planetesimal formation I: The impact of the planetesimal surface density in the terrestrial planet zone
• Towards a population synthesis of discs and planets. II. Confronting disc models and observations at the population level
• From Dust to Planets I: Planetesimal and Embryo Formation
• How does accretion of planet-forming disks influence stellar abundances?
• The impact of dynamic pressure bumps on the observational properties of protoplanetary disks
• Linking planetary embryo formation to planetesimal formation II: The impact of pebble accretion in the terrestrial planet zone
• Resilience of Planetesimal Formation in Weakly-Reinforced Pressure Bumps
• Linking planetesimal and dust content in protoplanetary disks via a local toy model
• Planetesimal formation at the gas pressure bump following a migrating planet I. Basic characteristics of the new formation model
• The formation of wide exoKuiper belts from migrating dust traps
• Dynamical avenues for Mercury's origin I: The lone survivor of a primordial generation of short-period proto-planets
• Making the Solar System
• The interplay between pebble and planetesimal accretion in population synthesis models and its role in giant planet formation
• On the multiple generations of planetary embryos
• Formation of pebbles in (gravito-)viscous protoplanetary disks with various turbulent strengths
• Gap opening by planets in discs with magnetised winds
• Growing the seeds of pebble accretion through planetesimal accretion
• High Resolution Study of Planetesimal Formation by Gravitational Collapse of Pebble Clouds
• Toward a Population Synthesis of Disks and Planets I. Evolution of Dust with Entrainment in Winds and Radiation Pressure
• Dust-Gas Coupling in Turbulence- and MHD Wind-Driven Protoplanetary Disks: Implications for Rocky Planet Formation
• Can the giant planets of the Solar System form via pebble accretion in a smooth protoplanetary disc?
• Planet formation and disk mass dependence in a pebble-driven scenario for low mass stars
• Constraining giant planet formation with synthetic ALMA images of the Solar System's natal protoplanetary disk
• A Pluto-Charon Sonata III. Growth of Charon from a Circum-Pluto Ring of Debris
• The CARMENES search for exoplanets around M dwarfs. Occurrence rates of Earth-like planets around very low-mass stars
• Formation of Multiple Dynamical Classes in the Kuiper Belt via Disk Dissipation
• The New Generation Planetary Population Synthesis (NGPPS). VII. Statistical comparison with the HARPS/Coralie survey
• Forming rocky exoplanets around K-dwarf stars
• Planetesimal Growth in Evolving Protoplanetary Disks: Constraints from the Pebble Supply
• How does the chemical composition of solids influence the formation of planetesimals?
• C/O ratios in self-gravitating protoplanetary discs with dust evolution
• The Prospects for Hurricane-like Vortices in Protoplanetary Disks
• Rapid Formation of Super-Earths Around Low-Mass Stars
• A large sub-Neptune transiting the thick-disk M4V TOI-2406