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The 13 pages that link to Restricted three-body problem, each with the reason it gives.

• Two-body problemCompared with: It adds a test particle without retaining the exact two-body dynamics.

• Three-body problemBroader topic: It simplifies the general problem while retaining rich orbital behavior.

• Lagrange pointNarrower topic: Lagrange points arise as equilibrium solutions of this model.

• Hill sphereNarrower topic: It supplies the dynamical framework used to define gravitational dominance.

• Tidal tailBroader topic: It approximates how stars move through the changing gravitational field of an encounter.

• Roche lobeNarrower topic: Its rotating-frame dynamics provide the standard framework for deriving Roche lobes.

• Trojan asteroidNarrower topic: It describes the dynamics that make Trojan regions possible.

• Halo orbitNarrower topic: Halo-orbit theory grew from periodic solutions of this classical celestial-mechanics problem.

• Orbital energyCompared with: In this time-dependent setting, ordinary two-body orbital energy is generally not conserved.

• Jupiter TrojanNarrower topic: It describes the dynamics underlying Jupiter’s stable Trojan regions.

• Kepler orbitCompared with: The extra gravitational source generally prevents a single fixed-focus Kepler conic from describing the path.

• Co-orbital configurationRelated: It provides the standard framework for analyzing Trojan and other co-orbital motion.

• Horseshoe orbitNarrower topic: It supplies the standard framework for describing a small object’s horseshoe motion around two primaries.