Giant planet formation at the pressure maxima of protoplanetary disks II. A hybrid accretion scenario

Abstract

Recent observations of protoplanetary disks have revealed ring-like structures that can be associated to pressure maxima. Pressure maxima are known to be dust collectors and planet migration traps. Most of planet formation works are based either on the pebble accretion model or on the planetesimal accretion model. However, recent studies proposed the possible formation of Jupiter by the hybrid accretion of pebbles and planetesimals. We aim to study the full process of planet formation consisting of dust evolution, planetesimal formation and planet growth at a pressure maximum in a protoplanetary disk. We compute, through numerical simulations, the gas and dust evolution, including dust growth, fragmentation, radial drift and particle accumulation at a pressure bump. We also consider the formation of planetesimals by streaming instability and the formation of a moon-size embryo that grows into a giant planet by the hybrid accretion of pebbles and planetesimals. We find that pressure maxima in protoplanetary disks are efficient collectors of dust drifting inwards. The condition of planetesimal formation by streaming instability is fulfilled due to the large amount of dust accumulated at the pressure bump. Then, a massive core is quickly formed (in $\sim 10^4$ yr) by the accretion of pebbles. After the pebble isolation mass is reached, the growth of the core slowly continues by the accretion of planetesimals. The energy released by planetesimal accretion delays the onset of runaway gas accretion, allowing a gas giant to form after $\sim$1 Myr of disk evolution. The pressure maximum also acts as a migration trap. Pressure maxima in protoplanetary disks are preferential locations for dust traps, planetesimal formation by streaming instability and planet migration traps. All these conditions allow the fast formation of a giant planet by the hybrid accretion of pebbles and planetesimals.

Accepted for publication in Astronomy & Astrophysics

References in corpus (35)

• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Separating gas-giant and ice-giant planets by halting pebble accretion
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Comparing Jupiter interior structure models to Juno gravity measurements and the role of a dilute core
• Planetesimal formation starts at the snow line
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Grain Retention and Formation of Planetesimals near the Snow Line in MRI-driven Turbulent Protoplanetary Disks
• Dust size distributions in coagulation/fragmentation equilibrium: Numerical solutions and analytical fits
• Close-in planetesimal formation by pile-up of drifting pebbles
• Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks
• Planetesimal formation around the snow line in MRI-driven turbulent protoplanetary disks
• Can dust coagulation trigger streaming instability?
• Planet formation with envelope enrichment: new insights on planetary diversity
• An Atmospheric Structure Equation for Grain Growth
• Can dead zones create structures like a transition disk?
• Embryos grown in the dead zone: Assembling the first protoplanetary cores in low mass self-gravitating circumstellar disks of gas and solids
• Coorbital thermal torques on low-mass protoplanets
• Improved torque formula for low and intermediate mass planetary migration
• Critical core mass for enriched envelopes: the role of H2O condensation
• Planet population synthesis driven by pebble accretion in cluster environments
• The opacity of grains in protoplanetary atmospheres
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• Planet formation by pebble accretion in ringed disks
• Ring formation and dust dynamics in wind-driven protoplanetary discs: global simulations
• Dust-driven viscous ring-instability in protoplanetary disks
• Spontaneous ring formation in wind-emitting accretion discs
• Growth after the streaming instability: from planetesimal accretion to pebble accretion
• Jupiter's heavy-element enrichment expected from formation models
• Rossby wave instability does not require sharp resistivity gradients
• Oligarchic planetesimal accretion and giant planet formation
• Thermal torque effects on the migration of growing low-mass planets
• The impact of pebble flux regulated planetesimal formation on giant planet formation
• X-ray photoevaporation's limited success in the formation of planetesimals by the streaming instability
• Setting the Stage: Planet formation and Volatile Delivery
• Planetesimal fragmentation and giant planet formation II: dependencies with planetesimal relative velocities and compositions

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• The Nature of the Radius Valley: Hints from Formation and Evolution Models
• How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
• Dust growth and evolution in protoplanetary disks
• How drifting and evaporating pebbles shape giant planets II: Volatiles and refractories in atmospheres
• Jupiter's inhomogeneous envelope
• How dust fragmentation may be beneficial to planetary growth by pebble accretion
• How planets grow by pebble accretion. III. Emergence of an interior composition gradient
• Efficient planet formation by pebble accretion in ALMA rings
• From super-Earths to sub-Neptunes: Observational constraints and connections to theoretical models
• A fading radius valley towards M-dwarfs, a persistent density valley across stellar types
• Rapid Formation of Massive Planetary Cores in a Pressure Bump
• Most super-Earths formed by dry pebble accretion are less massive than 5 Earth masses
• Giants are bullies: how their growth influences systems of inner sub-Neptunes and super-Earths
• The effect of a strong pressure bump in the Sun's natal disk: Terrestrial planet formation via planetesimal accretion rather than pebble accretion
• A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)
• Rapid Formation of Jupiter and Wide-Orbit Exoplanets in Disks with Pressure Bumps
• An Analytical Theory for the Growth from Planetesimals to Planets by Polydisperse Pebble Accretion
• The importance of thermal torques on the migration of planets growing by pebble accretion
• How planets grow by pebble accretion IV: Envelope opacity trends from sedimenting dust and pebbles
• Long live the disk: lifetimes of protoplanetary disks in hierarchical triple star systems and a possible explanation for HD 98800 B
• Sequential giant planet formation initiated by disc substructure
• The role of the drag force in the gravitational stability of dusty planet-forming disc -- II. Numerical simulations
• Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets
• On the multiple generations of planetary embryos
• Solving for the 2D Water Snowline with Hydrodynamic Simulations. Emergence of gas outflow, water cycle and temperature plateau
• Planetary core formation via multi-species pebble accretion
• Self-consistent ring model in protoplanetary disks: temperature dips and substructure formation
• Planetesimal and planet formation in transient dust traps
• The imprint of X-ray photoevaporation of planet-forming discs on the orbital distribution of giant planets -- II. Theoretical predictions
• Accreting luminous low-mass planets escape from migration traps at pressure bumps
• The role of density perturbation on planet formation by pebble accretion
• The influence of planetesimal fragmentation on planet formation
• The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-Driven Substructures Explaining the Diversity of Disk Morphologies
• Accretion of aerodynamically large pebbles
• Increased isolation mass for pebble accreting planetary cores in pressure maxima of protoplanetary discs
• The PAIRS project: a global formation model for planets in binaries. I. Effect of disc truncation on the growth of S-type planets
• A tension between dust and gas radii: the role of substructures and external photoevaporation in protoplanetary disks
• Characterization of the dust content in the ring around Sz 91: indications for planetesimal formation?