Stability of Distant Satellites of Giant Planets in the Solar System

Abstract

We conduct a systematic survey of the regions in which distant satellites can orbit stably around the four giant planets in the solar system, using orbital integrations of up to $10^9$ yr. In contrast to previous investigations, we use a grid of initial conditions on a surface of section to explore phase space uniformly inside and outside the planet's Hill sphere (radius $r_{\mathrm{H}}$; satellites outside the Hill sphere sometimes are also known as quasi-satellites). Our confirmations and extensions of old results and new findings include the following: (i) many prograde and retrograde satellites can survive out to radii $\sim 0.5r_{\mathrm{H}}$ and $\sim 0.7r_{\mathrm{H}}$, respectively, while some coplanar retrograde satellites of Jupiter and Neptune can survive out to $\sim r_{\mathrm{H}}$; (ii) stable orbits do not exist within the Hill sphere at high ecliptic inclinations when the semi-major axis is large enough that the solar tide is the dominant non-Keplerian perturbation; (iii) there is a gap between $\sim r_{\mathrm{H}}$ and $2r_{\mathrm{H}}$ in which no stable orbits exist; (iv) at distances $\gtrsim 2r_{\mathrm{H}}$ stable satellite orbits exist around Jupiter, Uranus and Neptune (but not Saturn). For Uranus and Neptune, in particular, stable orbits are found at distances as large as $\sim 10r_{\mathrm{H}}$; (v) the differences in the stable zones beyond the Hill sphere arise mainly from differences in the planet/Sun mass ratio and perturbations from other planets; in particular, the absence of stable satellites around Saturn is mainly due to perturbations from Jupiter. It is therefore likely that satellites at distances $\gtrsim 2r_{\mathrm{H}}$ could survive for the lifetime of the solar system around Uranus, Neptune, and perhaps Jupiter.

arXiv commentAJ in press; updated discussion and references

References in corpus (4)

• Irregular Satellites of the Planets: Products of Capture in the Early Solar System
• On the Secular Behavior of Irregular Satellites
• A Survey for "Normal" Irregular Satellites Around Neptune: Limits to Completeness
• Ultra Deep Survey for Irregular Satellites of Uranus: Limits to Completeness

Cited by in corpus (20)

• The Evolution of Wide Binary Stars
• STIS Coronagraphic Imaging of Fomalhaut: Main Belt Structure and the Orbit of Fomalhaut b
• The Kepler-19 System: A Transiting 2.2 R_Earth Planet and a Second Planet Detected via Transit Timing Variations
• $\beta$ Pictoris' inner disk in polarized light and new orbital parameters for $\beta$ Pictoris b
• The Orbit and Transit Prospects for $\beta$ Pictoris b constrained with One Milliarcsecond Astrometry
• Stability of prograde and retrograde planets in circular binary systems
• Application of the MEGNO technique to the dynamics of Jovian irregular satellites
• Collisional Evolution of Irregular Satellite Swarms: Detectable Dust around Solar System and Extrasolar Planets
• Wind-shearing in gaseous protoplanetary disks and the evolution of binary planetesimals
• Detecting exomoons from radial velocity measurements of self-luminous planets: application to observations of HR 7672 B and future prospects
• Transit of Exomoon Plasma Tori: New Diagnosis
• From order to chaos in Earth satellite orbits
• Fomalhaut b as a Cloud of Dust: Testing Aspects of Planet Formation Theory
• Dynamical evolution of thin dispersion-dominated planetesimal disks
• Lunar ejecta origin of near-Earth asteroid Kamo`oalewa is compatible with rare orbital pathways
• The dynamics of the elliptic Hill problem : Periodic orbits and stability regions
• On the Use of Cherenkov Telescopes for Outer Solar System Body Occultations
• Collisional Cascade Caclulations for Irregular Satellite Swarms in Fomalhaut b
• A Deep Search for Additional Satellites around the Dwarf Planet Haumea
• New Moons of Uranus and Neptune from Ultra-Deep Pencil Beam Surveys