Linked from

The 30 pages that link to Escape velocity, each with the reason it gives.

• VelocityBroader topic: It is a specific threshold velocity set by a gravitational field.

• Gravitational potentialRelated: Its energy condition compares kinetic energy with the potential relative to infinity.

• Orbital periodCompared with: An unbound trajectory has no repeating orbit and therefore no orbital period.

• Atmospheric escapeRelated: It sets the speed threshold that escaping atmospheric particles must overcome.

• Terminal velocityCompared with: It is a threshold speed for escape, not a steady speed set by fluid forces.

• Gravitational potential energyRelated: Escape speed follows from supplying enough kinetic energy to overcome gravitational binding energy.

• Gravitational binding energyRelated: It expresses the local energy threshold for escaping gravitational attraction.

• Vis-viva equationCompared with: It is the zero-energy boundary case of the vis-viva relation.

• Gravity assistRelated: The incoming and outgoing hyperbolic excess speeds are equal in an ideal unpowered flyby.

• Orbital decayCompared with: Orbital decay lowers orbital energy toward capture or impact, opposite the energy increase required for escape.

• SpeedRelated: It names a threshold speed for leaving a gravitational field.

• SpaceflightRelated: It captures the energy challenge of leaving Earth, though rockets can reach orbit below it.

• Hyperbolic trajectoryRelated: Exceeding local escape speed produces an unbound trajectory.

• Specific orbital energyCompared with: At a given distance, it marks the speed at which specific orbital energy reaches zero.

• Stellar kinematicsRelated: High-velocity stars help constrain the Milky Way’s gravitational binding.

• Schwarzschild radiusRelated: A Newtonian calculation gives the same radius by setting escape velocity equal to light speed, though general relativity supplies the correct account.

• Galactic windRelated: Comparing wind speed with the galaxy’s escape velocity helps determine whether gas can leave its halo.

• OrbitCompared with: At the boundary between bound and unbound motion, an object no longer returns on a closed orbit.

• Gravitational parameterRelated: Its value at a given distance depends directly on the body's μ.

• RocketRelated: Launch vehicles must supply enough velocity to reach orbit or leave a planet.

• Suborbital spaceflightRelated: Suborbital vehicles remain gravitationally bound rather than reaching escape trajectories.

• Circular orbitCompared with: Comparing it with circular-orbit speed clarifies the energy needed to leave a bound path.

• Konstantin TsiolkovskyRelated: His spaceflight calculations addressed the high speeds needed to leave Earth.

• Gravitationally bound systemRelated: It measures whether an object’s motion can carry it beyond a system’s gravitational hold.

• Stellar orbitRelated: Comparing a star’s speed with escape conditions helps distinguish bound paths from escape.

• Orbital energyCompared with: At the escape threshold, orbital energy changes from negative to zero.

• Orbital spaceflightCompared with: Reaching orbit requires less speed than escaping Earth, though both depend on gravity and motion.

• Equations for a falling bodyCompared with: It concerns gravity over large distances, unlike the near-surface constant-acceleration approximation.

• Potential wellCompared with: It expresses the classical threshold separating a trapped trajectory from escape.

• Robert Esnault-PelterieRelated: It expresses one of the basic physical thresholds that rocket-powered space travel must overcome.