Rapid formation of Gas Giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores

Abstract

Gas-giant planets, such as Jupiter, Saturn and massive exoplanets, were formed via the gas accretion onto the solid cores each with a mass of roughly ten Earth masses. However, rapid radial migration due to disk-planet interaction prevents the formation of such massive cores via planetesimal accretion. Comparably rapid core growth via pebble accretion requires very massive protoplanetary disks because most pebbles fall into the central star. Although planetesimal formation, planetary migration, and gas-giant core formation have been studied with much effort, the full evolution path from dust to planets are still uncertain. Here we report the result of full simulations for collisional evolution from dust to planets in a whole disk. Dust growth with realistic porosity allows the formation of icy planetesimals in the inner disk (> 10 au), while pebbles formed in the outer disk drift to the inner disk and there grow to planetesimals. The growth of those pebbles to planetesimals suppresses their radial drift and supplies small planetesimals sustainably in the vicinity of cores. This enables rapid formation of sufficiently massive planetary cores within 0.2-0.4 million years, prior to the planetary migration. Our models shows first gas giants form at 2-7 au in rather common protoplanetary disks, in agreement with the exoplanet and solar systems.

arXiv commentAccepted for publication in ApJ

References in corpus (29)

• Disk Frequencies and Lifetimes in Young Clusters
• Coagulation, fragmentation and radial motion of solid particles 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
• 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
• High Resolution Submillimeter Constraints on Circumstellar Disk Structure
• Protoplanetary Disk Structures in Ophiuchus II: Extension to Fainter Sources
• Planet Formation by Coagulation: A Focus on Uranus and Neptune
• Pebble isolation mass --- scaling law and implications for the formation of super-Earths and gas giants
• Fluffy dust forms icy planetesimals by static compression
• Hints for a Turnover at the Snow Line in the Giant Planet Occurrence Rate
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Modeling the Formation of Giant Planet Cores I: Evaluating Key Processes
• A record of planet migration in the Main Asteroid Belt
• How planetary growth outperforms migration
• Erosion and the limits to planetesimal growth
• Planetary Growth with Collisional Fragmentation and Gas Drag
• Planetary Core Formation with Collisional Fragmentation and Atmosphere to Form Gas Giant Planets
• A Balanced Budget View on Forming Giant Planets by Pebble Accretion
• The tensile strength of dust aggregates consisting of small elastic grains: Constraints on the size of condensates in protoplanetary disks
• Is water ice an efficient facilitator for dust coagulation?
• Catching drifting pebbles II. A stochastic equation of motions for pebbles
• Influences of three-dimensional gas flow induced by protoplanets on pebble accretion --$\mathrm{I}$. shear regime
• The Growth of Protoplanets via the Accretion of Small Bodies in Disks Perturbed by the Planetary Gravity
• Orbital evolution of planetesimals in gaseous disks
• The Mass Budgets and Spatial Scales of Exoplanet Systems and Protoplanetary Disks

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• Leaky dust traps: How fragmentation impacts dust filtering by planets
• How large are the monomers of dust aggregates in planet-forming disks?: Insights from quantitative optical and near-infrared polarimetry
• On the mass of gas giant planets: Is Saturn a failed gas giant?
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Observed polarized scattered light phase functions of planet-forming disks
• Formation of dust clumps with sub-Jupiter mass and cold shadowed region in gravitationally unstable disk around Class 0/I protostar in L1527 IRS
• Collisional Growth and Fragmentation of Dust Aggregates. II. Mass Distribution of Icy Fragments
• Grain Growth During Protostellar Disk Formation
• A low accretion efficiency of planetesimals formed at planetary gap edges
• No evidence of the significant grain growth but tentative discovery of disk substructure in a disk around the Class I Protostar L1489 IRS
• Heavy-element Accretion by Proto-Jupiter in a Massive Planetesimal Disk, Revisited
• The ultra narrow FRB20191107B, and the origins of FRB scattering
• Investigating the Bouncing Barrier with Collision Simulations of Compressed Dust Aggregates
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks II: Dust Ring Formation Mediated by Backreaction and Fragmentation
• Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I: First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
• The influence of planetesimal fragmentation on planet formation
• Giant planet formation via pebble accretion across different stellar masses
• Interparticle normal force in highly porous granular matter during compression
• A fast tree algorithm for multi-component coagulation equation
• Planetesimal gravitational collapse in a gaseous environment: Thermal and dynamic evolution