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The 69 pages that link to Hydrostatic equilibrium, each with the reason it gives.

• Stellar evolutionRelated: This balance supports a star against collapse during most of its life.

• Star formationRelated: Fusion-driven pressure eventually balances gravity and ends the protostar's main collapse.

• Hydrostatic pressureRelated: Its pressure-balance equation explains how hydrostatic pressure varies with height.

• Atmospheric pressureRelated: The balance between gravity and vertical pressure gradients describes how atmospheric pressure changes with height.

• White dwarfRelated: A stable white dwarf balances self-gravity with pressure from degenerate electrons.

• Accretion diskRelated: Pressure helps support a disk vertically against the central object's gravity.

• Main sequenceRelated: The balance between gravity and pressure lets core fusion sustain a stable main-sequence star.

• GravityRelated: It explains how gravity is balanced inside planets, stars, and atmospheres.

• Virial theoremCompared with: The virial theorem applies to global energy balance, while hydrostatic equilibrium describes local force balance.

• GeoidRelated: An idealized ocean at rest aligns its surface with an equipotential such as the geoid.

• Gravitational collapseCompared with: Collapse begins when this balance fails to support the matter.

• Atmosphere of EarthRelated: This balance explains the atmosphere’s vertical pressure structure.

• Proton–proton chainRelated: The chain’s energy helps maintain the pressure that supports the Sun against gravity.

• Atmospheric convectionRelated: Convection develops within an atmosphere whose background pressure generally balances gravity.

• Gravitational instabilityCompared with: It describes balanced configurations that remain stable against small disturbances.

• Stellar structureRelated: This balance sets the pressure gradient that supports a star against its own gravity.

• PlanetRelated: This balance explains why sufficiently massive planets become nearly round.

• Stellar atmosphereRelated: It describes how pressure supports much of a star’s atmosphere against gravity.

• Stellar massRelated: A star’s mass determines the gravitational load that internal pressure must support.

• Electron degeneracy pressureRelated: In a white dwarf, degeneracy pressure supplies the gradient that balances gravity.

• AstrophysicsRelated: This balance explains why many stars remain stable for long periods.

• Dwarf planetRelated: This physical condition underlies the definition's requirement that a body be nearly round.

• Intracluster mediumRelated: This balance lets X-ray observations estimate the cluster’s gravitational mass.

• CeresRelated: Ceres is round enough for this balance to support its dwarf-planet classification.

• HydrostaticsRelated: It states the force balance that keeps a fluid at rest.

• Planetary atmosphereRelated: Atmospheric pressure generally falls with altitude because it supports the weight of overlying gas.

• Pressure gradientCompared with: It demonstrates that a pressure gradient can balance gravity without producing flow.

• SunRelated: This balance keeps the Sun from collapsing or rapidly expanding.

• Solar nebulaRelated: This balance emerged as the collapsing central region became the Sun.

• Coma ClusterRelated: It is used to interpret the pressure and temperature structure of Coma's hot gas.

• Air densityRelated: The vertical air-density profile is tied to the pressure decrease that balances atmospheric weight.

• AsteroseismologyRelated: It defines the equilibrium state around which stellar oscillations occur.

• Chandrasekhar limitNarrower topic: The limit marks the loss of a stable equilibrium between pressure and gravity.

• PachyostosisRelated: Added bone mass can help aquatic vertebrates balance buoyant forces.

• Pressure-gradient forceCompared with: Unlike horizontal pressure-driven flow, vertical air pressure gradients usually balance gravity.

• Convection zoneRelated: This balance sets the pressure and density background through which convection develops.

• Gas giantRelated: It governs the balance between gravity and pressure throughout a gas giant.

• Rayleigh–Taylor instabilityCompared with: The instability begins when acceleration makes a density-stratified equilibrium unfavorable.

• Thermal windRelated: Combined with geostrophic balance, it yields the thermal-wind relation.

• Radiative zoneRelated: This balance sets the pressure and density profile through the zone.

• Subrahmanyan ChandrasekharRelated: His stellar models tested whether internal pressure could balance gravity at different masses.

• Helium burningRelated: Energy from helium fusion helps maintain this balance in a stable burning core.

• Planetary massRelated: A planet’s mass contributes to the pressure balancing gravity inside it.

• Eddington luminosityNarrower topic: The Eddington balance is a radiative contribution to support against gravitational collapse.

• HaumeaRelated: Haumea’s shape has been used to assess whether its interior relaxed under self-gravity.

• Pre-main-sequence starRelated: A pre-main-sequence star is largely in this balance even while it continues to contract and radiate.

• Tolman–Oppenheimer–Volkoff limitRelated: The limit marks where relativistic hydrostatic support no longer yields a stable configuration.

• Alexis ClairautRelated: A rotating fluid Earth’s equilibrium shape depends on this balance.

• ExosphereRelated: Below the exobase, collisions help maintain the fluid-like balance used in atmospheric models.

• Kelvin–Helmholtz mechanismRelated: A contracting star adjusts its pressure to remain near this balance.