The consequences of planetary migration on the minor bodies of the early Solar System

Abstract

Pebble accretion is an efficient mechanism able to build up the core of the giant planets within the lifetime of the protoplanetary disc gas-phase. The core grows via this process until the protoplanet reaches its pebble isolation mass and starts to accrete gas. During the growth, the protoplanet undergoes a rapid, large-scale, inward migration due to the interactions with the gaseous protoplanetary disc. In our work, we investigate how this early migration would have affected the minor body populations in our solar system. In particular, we focus on the Jupiter Trojans and the Hildas asteroids. We found that a massive and eccentric Hilda group is captured during the migration from a region between 5 and 8 au and subsequently depleted during the late instability of the giant planets. Our simulations also show that inward migration of the giant planets always produces a Jupiter Trojans' leading swarm more populated than the trailing one, with a ratio comparable to the current observed Trojan asymmetry ratio. The in situ formation of Jupiter, on the other hand, produces symmetric leading/trailing swarms. The reason for the asymmetry is the relative drift between the migrating planet and the particles in the coorbital resonance. The capture happens during the growth of Jupiter's core and Trojan asteroids are afterwards carried along during the giant planet's migration to their final orbits. The asymmetry and eccentricity of the captured Trojans correspond well to observations, but their inclinations are near zero and their total mass is 3-4 orders of magnitude higher than the current population. Future modelling will be needed to understand whether the dynamical evolution of the Trojans over billions of years will raise the inclinations and deplete the masses to observed values.

arXiv comment19 pages, 21 figures. Accepted for publication in A&A

References in corpus (48)

• A low mass for Mars from Jupiter's early gas-driven migration
• Streaming Instabilities in Protoplanetary Disks
• Rapid growth of gas-giant cores by pebble accretion
• A simple model for the evolution of the dust population in protoplanetary disks
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
• 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
• THE ORIGIN OF PLUTO'S ORBIT: IMPLICATIONS FOR THE SOLAR SYSTEM BEYOND NEPTUNE
• Solar System evolution from compositional mapping of the asteroid belt
• Protoplanetary Disk Turbulence Driven by the Streaming Instability: Non-Linear Saturation and Particle Concentration
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Separating gas-giant and ice-giant planets by halting pebble accretion
• Rapid Coagulation of Porous Dust Aggregates Outside the Snow Line: A Pathway to Successful Icy Planetesimal Formation
• Reversing type II migration: resonance trapping of a lighter giant protoplanet
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Dynamics of the giant planets of the solar system in the gaseous proto-planetary disk and relationship to the current orbital architecture
• Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
• Growing the gas-giant planets by the gradual accumulation of pebbles
• Planetesimal formation near the snowline: in or out?
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
• Capture of Trojans by Jumping Jupiter
• Evidence from the asteroid belt for a violent past evolution of Jupiter's orbit
• Planetesimal formation by sweep-up: How the bouncing barrier can be beneficial to growth
• Large grains in the disk of CQ Tau
• Fast accretion of small planetesimals by protoplanetary cores
• Modeling the Formation of Giant Planet Cores I: Evaluating Key Processes
• A record of planet migration in the Main Asteroid Belt
• Dynamical erosion of the asteroid belt and implications for large impacts in the inner solar system
• Towards Planetesimals in the Disk around TW Hya: 3.5 centimeter Dust Emission
• The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
• Young Solar System's Fifth Giant Planet?
• Constraints on resonant-trapping for two planets embedded in a protoplanetary disc
• Breaking through: The effects of a velocity distribution on barriers to dust growth
• Evolution of Planetary Systems in Resonance
• WISE/NEOWISE Observations of the Jovian Trojans: Preliminary Results
• The Properties of Jovian Trojan Asteroids Listed in SDSS Moving Object Catalog 3
• On the origin of the Trojan asteroids: Effects of Jupiter's mass accretion and radial migration
• The evolution of asteroids in the jumping-Jupiter migration model
• The formation of mini-Neptunes
• The growth of planets by pebble accretion in evolving protoplanetary discs
• The Trojan Color Conundrum
• Ridge Formation and De-Spinning of Iapetus via an Impact-Generated Satellite
• The effect of planetary migration on the corotation resonance
• The Formation of Jupiter, the Jovian Early Bombardment and the Delivery of Water to the Asteroid Belt: The Case of (4) Vesta
• The color-magnitude distribution of Hilda asteroids: Comparison with Jupiter Trojans
• Size Distribution of Small Hilda Asteroids
• Asteroid 4 Vesta: dynamical and collisional evolution during the Late Heavy Bombardment

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