The Great Inequality and the Dynamical Disintegration of the Outer Solar System

Abstract

Using an ensemble of N-body simulations, this paper considers the fate of the outer gas giants (Jupiter, Saturn, Uranus, and Neptune) after the Sun leaves the main sequence and completes its stellar evolution. Due to solar mass-loss -- which is expected to remove roughly half of the star's mass -- the orbits of the giant planets expand. This adiabatic process maintains the orbital period ratios, but the mutual interactions between planets and the width of mean-motion resonances (MMR) increase, leading to the capture of Jupiter and Saturn into a stable 5:2 resonant configuration. The expanded orbits, coupled with the large-amplitude librations of the critical MMR angle, make the system more susceptible to perturbations from stellar flyby interactions. Accordingly, within about 30 Gyr, stellar encounters perturb the planets onto the chaotic sub-domain of the 5:2 resonance, triggering a large-scale instability, which culminates in the ejections of all but one planet over the subsequent $\sim 10$ Gyr. After an additional $\sim 50$ Gyr, a close stellar encounter (with a perihelion distance less than $\sim 200$ AU) liberates the final planet. Through this sequence of events, the characteristic timescale over which the solar system will be completely dissolved is roughly 100 Gyr. Our analysis thus indicates that the expected dynamical lifetime of the solar system is much longer than the current age of the universe, but is significantly shorter than previous estimates.

arXiv comment12 pages, 5 figures; accepted for publication in AJ

References in corpus (27)

• On the variation of the Initial Mass Function
• A Survey of Stellar Families: Multiplicity of Solar-Type Stars
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
• Stellar Multiplicity
• REBOUND: An open-source multi-purpose N-body code for collisional dynamics
• IAS15: A fast, adaptive, high-order integrator for gravitational dynamics, accurate to machine precision over a billion orbits
• Riding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks
• The spatial structure of mono-abundance sub-populations of the Milky Way disk
• No large population of unbound or wide-orbit Jupiter-mass planets
• A Dying Universe: The Long Term Fate and Evolution of Astrophysical Objects
• Stars, Gas, and Dark Matter in the Solar Neighborhood
• Distant future of the Sun and Earth revisited
• The Great Escape: How Exoplanets and Smaller Bodies Desert Dying Stars
• Chaotic diffusion in the Solar System
• The Origin of Chaos in the Outer Solar System
• Theory of Secular Chaos and Mercury's Orbit
• Cross Sections for Planetary Systems Interacting with Passing Stars and Binaries
• On the Dynamical Stability of the Solar System
• Quantifying stellar radial migration in an N-body simulation: blurring, churning, and the outer regions of galaxy discs
• Chaotic Disintegration of the Inner Solar System
• The Solar System's Post-Main Sequence Escape Boundary
• Hill stability in the AMD framework
• A simple model of the chaotic eccentricity of Mercury
• Dynamics of Planetary Systems Within Star Clusters: Aspects of the Solar System's Early Evolution
• Evolution of Planetary Systems with Time Dependent Stellar Mass Loss
• Dynamic stability of the Solar System: Statistically inconclusive results from ensemble integrations
• The rate of stellar encounters along a migrating orbit of the Sun

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• Disentangling the parameter space: The role of planet multiplicity in triggering dynamical instabilities on planetary systems around white dwarfs
• The Fate of Oceans on First-Generation Planets Orbiting White Dwarfs
• Rendez-vous with massive interstellar objects, as triggers of destabilisation
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• Simulation of images of protoplanetary disks after collision with free-floating planets
• Survival and dynamics of rings of co-orbital planets under perturbations
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