Linked from

The 25 pages that link to Two-body problem, each with the reason it gives.

• Kepler's laws of planetary motionRelated: Kepler's laws describe the idealized solution when only the Sun and one planet interact.

• Orbital mechanicsBroader topic: Its exact solutions provide the basic model for most introductory orbit calculations.

• Celestial mechanicsBroader topic: Its exact solution provides the baseline for orbital calculations.

• Roche limitRelated: The Roche limit extends simple orbital reasoning to a deformable satellite in a larger body's field.

• Three-body problemCompared with: Its exact solution shows the sharp contrast with three mutually interacting bodies.

• Orbit determinationRelated: It supplies the simplest dynamical model for propagating an estimated orbit.

• Gravity assistNarrower topic: A flyby’s basic geometry is often analyzed as a two-body encounter.

• Gravitational perturbationCompared with: Perturbations arise when real systems include influences excluded from this idealization.

• Orbital perturbationNarrower topic: Perturbations are departures from this idealized baseline.

• Semimajor axisNarrower topic: In the gravitational two-body solution, the relative orbit has a well-defined semimajor axis.

• Specific orbital energyNarrower topic: The familiar constant-energy formula follows from this idealized system.

• Reduced massNarrower topic: Reduced mass converts its relative-motion part into a one-body problem.

• Gravitational parameterNarrower topic: In this model, the relative orbit is governed by the sum of both bodies' gravitational parameters.

• Circular orbitNarrower topic: Circular orbits are exact solutions under the two-body idealization.

• Kepler's third lawNarrower topic: Its exact solution explains how the law applies when both orbiting bodies have significant mass.

• Stellar dynamicsBroader topic: It supplies the orbital baseline before additional stars perturb a system.

• Central forceRelated: Many central-force problems reduce to relative motion in a single effective particle.

• Gravitationally bound systemBroader topic: It gives the simplest exact model of a gravitationally bound pair.

• Jacobi integralCompared with: This simpler problem conserves ordinary orbital energy rather than requiring the rotating-frame Jacobi integral.

• Orbital precessionNarrower topic: It supplies the fixed-orbit baseline from which precession is measured.

• Orbit of the MoonRelated: It approximates Earth and Moon motion before solar perturbations are added.

• Kepler orbitNarrower topic: Its exact Newtonian solution produces Kepler orbits for motion relative to the system's center of mass.

• Kepler's first lawNarrower topic: The idealized Sun–planet system is a case of this solvable problem.

• Orbital station-keepingNarrower topic: It supplies the baseline orbit from which real perturbations are measured.

• Newtonian dynamicsBroader topic: It yields the idealized orbital motion of bodies such as planets and satellites.