The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation

Abstract

The solar system's dynamical state can be explained by an orbital instability among the giant planets. A recent model has proposed that the giant planet instability happened during terrestrial planet formation. This scenario has been shown to match the inner solar system by stunting Mars' growth and preventing planet formation in the asteroid belt. Here we present a large sample of new simulations of the "Early Instability" scenario. We use an N-body integration scheme that accounts for collisional fragmentation, and also perform a large set of control simulations that do not include an early giant planet instability. Since the total particle number decreases slower when collisional fragmentation is accounted for, the growing planets' orbits are damped more strongly via dynamical friction and encounters with small bodies that dissipate angular momentum (eg: hit-and-run impacts). Compared with simulations without collisional fragmentation, our fully evolved systems provide better matches to the solar system's terrestrial planets in terms of their compact mass distribution and dynamically cold orbits. Collisional processes also tend to lengthen the dynamical accretion timescales of Earth analogs, and shorten those of Mars analogs. This yields systems with relative growth timescales more consistent with those inferred from isotopic dating. Accounting for fragmentation is thus supremely important for any successful evolutionary model of the inner solar system.

arXiv comment16 pages, 7 figures, 4 tables, accepted for publication in Icarus

References in corpus (65)

• Disk Frequencies and Lifetimes in Young Clusters
• Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics
• A low mass for Mars from Jupiter's early gas-driven migration
• Cometary Origin of the Zodiacal Cloud and Carbonaceous Micrometeorites
• THE ORIGIN OF PLUTO'S ORBIT: IMPLICATIONS FOR THE SOLAR SYSTEM BEYOND NEPTUNE
• Building Terrestrial Planets
• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Making other Earths: Dynamical Simulations of Terrestrial Planet Formation and Water Delivery
• Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
• Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water
• High-resolution simulations of the final assembly of Earth-like planets 1: terrestrial accretion and dynamics
• Statistical Study of the Early Solar System's Instability with 4, 5 and 6 Giant Planets
• Reversing type II migration: resonance trapping of a lighter giant protoplanet
• On the orbital evolution and growth of protoplanets embedded in a gaseous disc
• Formation of the Terrestrial Planets from a Narrow Annulus
• Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
• The timeline of the Lunar bombardment - revisited
• Growing the gas-giant planets by the gradual accumulation of pebbles
• Highly Siderophile Elements in the Earth's Mantle as a Clock for the Moon-forming Impact
• Capture of Trojans by Jumping Jupiter
• Close-in planetesimal formation by pile-up of drifting pebbles
• The Different Evolution of Gas and Dust in Disks around Sun-like and Cool Stars
• The Last Gasp of Gas Giant Planet Formation: A Spitzer Study of the 5 Myr-old Cluster NGC 2362
• Growing the terrestrial planets from the gradual accumulation of sub-meter sized objects
• Challenges in Planet Formation
• Mars' Growth Stunted by an Early Giant Planet Instability
• The Evidence for Slow Migration of Neptune from the Inclination Distribution of Kuiper Belt Objects
• Young Solar System's Fifth Giant Planet?
• Merging Criteria for Giant Impacts of Protoplanets
• Introducing the Eulalia and new Polana asteroid families: re-assessing primitive asteroid families in the inner Main Belt
• Constructing the secular architecture of the solar system II: The terrestrial planets
• Cataclysm no more: New views on the timing and delivery of lunar impactors
• Jumping Neptune Can Explain the Kuiper Belt Kernel
• The Frequency of Giant impacts on Earth-like Worlds
• On the Migration of Jupiter and Saturn: Constraints from Linear Models of Secular Resonant Coupling with the Terrestrial Planets
• Origin of Earth's water: sources and constraints
• Characterizing Exoplanet Habitability
• Solar System Formation in the Context of Extra-Solar Planets
• Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt
• The Feeding Zones of Terrestrial Planets and Insights into Moon Formation
• Compositional evolution during rocky protoplanet accretion
• Terrestrial Planet Formation in a protoplanetary disk with a local mass depletion: A successful scenario for the formation of Mars
• The Fragility of the Terrestrial Planets During a Giant Planet Instability
• A Collisional Origin to Earth's Non-chondritic Composition?
• Dynamical Shakeup of Planetary Systems II. N-body simulations of Solar System terrestrial planet formation induced by secular resonance sweeping
• Outward migration of Jupiter and Saturn in 3:2 or 2:1 resonance in radiative disks: implications for the Grand Tack and Nice models
• Late veneer and late accretion to the terrestrial planets
• The Effect of an Early Planetesimal-Driven Migration of the Giant Planets on Terrestrial Planet Formation
• Dynamical and collisional constraints on a stochastic late veneer on the terrestrial planets
• Analysis of terrestrial planet formation by the Grand Tack model: System architecture and tack location
• Terrestrial Planet Formation from an Annulus
• Constraining the primordial orbits of the Terrestrial Planets
• The excitation of a primordial cold asteroid belt as an outcome of the planetary instability
• Terrestrial Planet Formation During the Migration and Resonance Crossings of the Giant Planets
• Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?
• The common origin of family and non-family asteroids
• Earth-like Habitats in Planetary Systems
• Numerically Predicted Indirect Signatures of Terrestrial Planet Formation
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• Systematic mischaracterization of exoplanetary system dynamical histories from a model degeneracy near mean-motion resonance
• Jumping Jupiter can explain Mercury's orbit
• Stability of resonant configurations during the migration of planets and constraints on disk-planet interactions
• Collisional Fragmentation is Not a Barrier to Close-in Planet Formation
• Prevalance of Chaos in Planetary Systems Formed Through Embryo Accretion
• Evidence for Very Early Migration of the Solar System Planets from the Patroclus-Menoetius binary Jupiter Trojan

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• Origin of Earth's water: sources and constraints
• Characterizing Exoplanet Habitability
• Solar System Formation in the Context of Extra-Solar Planets
• Dynamical evidence for an early giant planet instability
• Onset of giant planet migration before 4480 million years ago
• A Tale of Planet Formation: From Dust to Planets
• Solar System Physics for Exoplanet Research
• Formation of Venus, Earth and Mars: Constrained by isotopes
• Realistic On-the-fly Outcomes of Planetary Collisions II: Bringing Machine Learning to N-body Simulations
• Born eccentric: constraints on Jupiter and Saturn's pre-instability orbits
• A record of the final phase of giant planet migration fossilized in the asteroid belt's orbital structure
• Growing Mars fast: High-resolution GPU simulations of embryo formation
• The Fundamental Connections Between the Solar System and Exoplanetary Science
• Dynamical Constraints on Mercury's Collisional Origin
• Evolution of the Earth's Atmosphere during Late Veneer Accretion
• Constraining the Formation of the Four Terrestrial Planets in the Solar System
• The "Breaking The Chains" migration model for super-Earths formation: the effect of collisional fragmentation
• Migration processes in the Solar System and their role in the evolution of the Earth and planets
• Reduced late bombardment on rocky exoplanets around M-dwarfs
• The effect of pre-impact spin on the Moon-forming collision
• Direct measurement of decimeter-sized rocky material in the Oort cloud
• Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants
• Dynamical avenues for Mercury's origin I: The lone survivor of a primordial generation of short-period proto-planets
• Origin and dynamical evolution of the asteroid belt
• Born extra-eccentric: A broad spectrum of primordial configurations of the gas giants that match their present-day orbits
• The Dissipation of the Solar Nebula Constrained by Impacts and Core Cooling in Planetesimals
• The early instability scenario: Mars' mass explained by Jupiter's orbit
• Dynamical avenues for Mercury's origin II: in-situ formation in the inner terrestrial disk
• The origins of nearly coplanar, non-resonant systems of close-in super-Earths
• Effects of pebble accretion on the growth and composition of planetesimals in the inner Solar System
• Explaining Mercury via a single giant impact is highly unlikely
• Modification of the composition and density of Mercury from late accretion
• Migration of pairs of giant planets in low-viscosity discs
• Can a jumping-Jupiter trigger the Moon's formation impact?
• Rethinking the role of the giant planet instability in terrestrial planet formation models
• Probabilities of collisions of planetesimals from different regions of the feeding zone of the terrestrial planets with the forming planets and the Moon
• A Pluto--Charon Sonata: Dynamical Limits on the Masses of the Small Satellites
• Importance of Giant Impact Ejecta for Orbits of Planets Formed during the Giant Impact Era
• Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation
• Mercury's formation within the Early Instability Scenario
• How much water was delivered from the asteroid belt to the Earth after its formation?
• Building Terrestrial Planets: Why results of perfect-merging simulations are not quantitatively reliable approximations to accurate modeling of terrestrial planet formation
• Protoplanet Collisions: Statistical Properties of Ejecta
• Can narrow disks in the inner solar system explain the four terrestrial planets?
• Residual Neural Networks for the Prediction of Planetary Collision Outcomes
• Crash Chronicles: relative contribution from comets and carbonaceous asteroids to Earth's volatile budget in the context of an Early Instability
• Impact-induced Vaporization During Accretion of Planetary Bodies
• Collisional Growth Within the Solar System's Primordial Planetesimal Disk and the Timing of the Giant Planet Instability
• iSyMBA: A Symplectic Massive Bodies Integrator with Planets Interpolation
• Terrestrial planet formation during giant planet formation and giant planet migration I: The first 5 million years
• Planet formation: key mechanisms and global models
• Protoplanet collisions: new scaling laws from SPH simulations
• Motion of Planetesimals in the Hill Sphere of the Star Proxima Centauri
• Probabilities of collisions of bodies ejected from forming Earth with the terrestrial planets
• The Moon-forming Impact as a Constraint for the Inner Solar System's Formation
• Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery
• Predicting the Dominant Formation Mechanism of Multi-Planetary Systems
• Water worlds in N-body simulations with fragmentation in systems without gaseous giants
• Realistic outcomes of moon-moon collisions in Lunar formation theory
• Stability of a cluster-disrupted mean-motion resonance (chain) in HR 8799 and PDS 70
• Migration of celestial bodies in the Solar system and in several exoplanetary systems
• Acceleration of planetary migration: Resonance crossing and planetesimal ring
• Magnitude of stable iron isotope fractionation limited by multiple stages of terrestrial core formation