Dynamical evidence for an early giant planet instability
arXiv:1912.10879 · doi:10.1016/j.icarus.2019.113605
Abstract
The dynamical structure of the Solar System can be explained by a period of orbital instability experienced by the giant planets. While a late instability was originally proposed to explain the Late Heavy Bombardment, recent work favors an early instability. We model the early dynamical evolution of the outer Solar System to self-consistently constrain the most likely timing of the instability. We first simulate the dynamical sculpting of the primordial outer planetesimal disk during the accretion of Uranus and Neptune from migrating planetary embryos during the gas disk phase, and determine the separation between Neptune and the inner edge of the planetesimal disk. We performed simulations with a range of migration histories for Jupiter. We find that, unless Jupiter migrated inwards by 10 AU or more, the instability almost certainly happened within 100 Myr of the start of Solar System formation. There are two distinct possible instability triggers. The first is an instability that is triggered by the planets themselves, with no appreciable influence from the planetesimal disk. Of those, the median instability time is Myr. Among self-stable systems -- where the planets are locked in a resonant chain that remains stable in the absence of a planetesimal's disk-- our self-consistently sculpted planetesimal disks nonetheless trigger a giant planet instability with a median instability time of 37-62 Myr for a reasonable range of migration histories of Jupiter. The simulations that give the latest instability times are those that invoked long-range inward migration of Jupiter from 15 AU or beyond; however these simulations over-excited the inclinations of Kuiper belt objects and are inconsistent with the present-day Solar System. We conclude on dynamical grounds that the giant planet instability is likely to have occurred early in Solar System history.
46 pages, 26 figures, Article reference YICAR_113605, https://authors.elsevier.com/tracking/article/details.do?aid=113605&jid=YICAR&surname=Ribeiro
References in corpus (25)
- Dynamical Outcomes of Planet-Planet Scattering
- Origins of Eccentric Extrasolar Planets: Testing the Planet-Planet Scattering Model
- Separating gas-giant and ice-giant planets by halting pebble accretion
- 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
- Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
- The timeline of the Lunar bombardment - revisited
- Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
- Exotic Earths: Forming Habitable Worlds with Giant Planet Migration
- Cavity opening by a giant planet in a protoplanetary disc and effects on planetary migration
- Constraints on resonant-trapping for two planets embedded in a protoplanetary disc
- On disc protoplanet interactions in a non-barotropic disc with thermal diffusion
- Gas giant planets as dynamical barriers to inward-migrating super-Earths
- The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
- Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion and disc evolution
- Constraining the giant planets' initial configuration from their evolution: implications for the timing of the planetary instability
- Disk Dispersal and Planet Formation Time Scales
- Outward migration of Jupiter and Saturn in 3:2 or 2:1 resonance in radiative disks: implications for the Grand Tack and Nice models
- The Grand Tack model: a critical review
- Modeling the Historical Flux of Planetary Impactors
- Planetesimal-driven planet migration in the presence of a gas disk
- Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?
- Extrasolar Planet Eccentricities from Scattering in the Presence of Residual Gas Disks
- Runaway gas accretion and gap opening versus type~I migration
- Instabilities in the Early Solar System due to a Self-gravitating Disk
Cited by in corpus (25)
- Early Solar System instability triggered by dispersal of the gaseous disk
- The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
- Growing Mars fast: High-resolution GPU simulations of embryo formation
- The terrestrial planet formation paradox inferred from high-resolution N-body simulations
- An interstellar origin for high-inclination Centaurs
- Did Mars possess a dense atmosphere during the first ~400 million years?
- Born extra-eccentric: A broad spectrum of primordial configurations of the gas giants that match their present-day orbits
- Implications of Jupiter Inward Gas-Driven Migration for the Inner Solar System
- Survivor bias: divergent fates of the Solar System's ejected vs. persisting planetesimals
- Hint of an exocomet transit in the CHEOPS lightcurve of HD 172555
- 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
- A race against the clock: Constraining the timing of cometary bombardment relative to Earth's growth
- Origin of Water in the Terrestrial Planets: Insights from Meteorite Data and Planet Formation Models
- Collision Chains among the Terrestrial Planets. II. An Asymmetry between Earth and Venus
- Effects of early intense bombardment on megaregolith evolution and on lunar (and planetary) surface samples
- Rethinking the role of the giant planet instability in terrestrial planet formation models
- Mercury's formation within the Early Instability Scenario
- Mars' formation can constrain the primordial orbits of the gas giants
- Can narrow disks in the inner solar system explain the four terrestrial planets?
- Can the orbital distribution of Neptune's 3:2 mean motion resonance result from stability sculpting?
- Crash Chronicles: relative contribution from comets and carbonaceous asteroids to Earth's volatile budget in the context of an Early Instability
- Collisional Growth Within the Solar System's Primordial Planetesimal Disk and the Timing of the Giant Planet Instability
- Collisional heating of icy planetesimals. I. Catastrophic collisions
- Protoplanetary disk formation from the collapse of a prestellar core