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The 64 pages that link to White dwarf, each with the reason it gives.

• Stellar evolutionBroader topic: Stars that lose their outer layers without a core-collapse supernova commonly end this way.

• Hydrostatic equilibriumBroader topic: It is a dense example of stellar hydrostatic support with a quantum-mechanical pressure source.

• Neutron starCompared with: White dwarfs are less dense remnants supported by electrons rather than neutron-rich matter.

• Pauli exclusion principleBroader topic: Its stability is a macroscopic consequence of electrons obeying exclusion.

• Type Ia supernovaNarrower topic: The exploding star is a white dwarf whose carbon- and oxygen-rich material undergoes thermonuclear burning.

• Black holeCompared with: It is a stable endpoint for many stars, rather than an object with an event horizon.

• SupernovaRelated: A white dwarf can undergo a thermonuclear explosion in a Type Ia event.

• FermionBroader topic: It is a macroscopic consequence of electron exclusion.

• Main sequenceCompared with: White dwarfs are the cooled remnants of many stars that once occupied the main sequence.

• PulsarCompared with: White dwarfs are less compact stellar remnants and do not produce the defining neutron-star pulsar mechanism.

• Hertzsprung–Russell diagramBroader topic: Its small emitting surface makes it faint despite its high surface temperature.

• Fermi–Dirac statisticsBroader topic: Its pressure arises from fermions filling states according to exclusion, even at low temperature.

• Planetary nebulaRelated: The hot central remnant remains after the surrounding gas has dispersed.

• Gravitational collapseBroader topic: Collapse halts at a white dwarf when electron degeneracy pressure supports the remnant.

• Red giantRelated: Low- and intermediate-mass stars end their evolution as white dwarfs after shedding their outer layers.

• Stellar massRelated: Stars below the threshold for core collapse typically end as white dwarfs.

• Color–magnitude diagramRelated: White dwarfs occupy a distinct faint region whose cooling sequence can constrain ages.

• Electron degeneracy pressureBroader topic: It is the clearest astronomical example of a star supported by degenerate electrons.

• Asymptotic giant branchRelated: Envelope ejection leaves the exposed core to cool as a white dwarf.

• Gravitational redshiftBroader topic: Its strong surface gravity produces a measurable redshift in emitted spectral lines.

• Ultraviolet astronomyRelated: Many white dwarfs emit strongly in ultraviolet light, exposing their temperatures and atmospheric composition.

• SiriusNarrower topic: Sirius B is a nearby example of this stellar remnant.

• Spin–statistics theoremRelated: Fermionic electron statistics supply the pressure that supports the star.

• X-ray binaryCompared with: Accreting white dwarfs produce cataclysmic variables rather than classical X-ray binaries.

• Chandrasekhar limitNarrower topic: The limit describes the maximum mass of this class of stellar remnant.

• Red dwarfCompared with: Despite the similar name, a white dwarf is a stellar remnant, not a hydrogen-fusing red dwarf.

• Fermi gasRelated: Its support illustrates the astrophysical effects of a degenerate Fermi gas.

• Stellar rotationBroader topic: Its rotation reflects angular-momentum evolution through the star’s later life and possible binary interactions.

• StarBroader topic: Most stars end as white dwarfs after shedding their outer layers.

• Subrahmanyan ChandrasekharBroader topic: His early work established a mass limit for these remnants.

• Mass–luminosity relationCompared with: White dwarfs have a different mass–luminosity behavior from hydrogen-burning main-sequence stars.

• Millisecond pulsarCompared with: Some rapidly pulsing white dwarfs resemble pulsars observationally but are not neutron stars.

• Neutron degeneracy pressureCompared with: It provides a lower-density stellar comparison in which electrons, not neutrons, supply degeneracy pressure.

• O-type starCompared with: White dwarfs are evolutionary remnants, not the massive hydrogen-burning stars classified as O type.

• Heat death of the universeBroader topic: White dwarfs are among the long-lived remnants expected after ordinary star formation ends.

• Ring NebulaRelated: The hot central remnant supplies radiation that ionizes the Ring Nebula's gas.

• Stellar coreRelated: A low- or intermediate-mass star leaves its exposed core as this remnant.

• Henry Norris RussellBroader topic: Russell helped establish that some faint, hot stars form a distinct class of stellar objects.

• Quantum degeneracyRelated: Electron degeneracy lets a white dwarf resist collapse despite intense compression.

• Cat's Eye NebulaRelated: The central star is evolving toward the white-dwarf state.

• Kelvin–Helmholtz mechanismRelated: Its cooling history is not powered by continuing Kelvin–Helmholtz contraction in the same way as a young star.

• Degenerate matterBroader topic: It is the clearest astronomical example of electron-degenerate matter.

• Quark starCompared with: It illustrates the much lower density and different support mechanism of an earlier compact-star stage.

• Cataclysmic variable starBroader topic: It is the compact accretor at the center of a cataclysmic variable.

• Cyclotron radiationRelated: Magnetic white dwarfs can show cyclotron features from accreting plasma.

• Giant starCompared with: Low- and intermediate-mass giants can leave white dwarfs after shedding their envelopes.

• Stellar astronomyBroader topic: White dwarfs are the common endpoint of stars that do not undergo core collapse.

• Carbon burningCompared with: Many lower-mass stars leave carbon-oxygen remnants without ever igniting carbon in their cores.

• Kepler's SupernovaRelated: A white dwarf’s thermonuclear disruption is the leading explanation for this supernova.

• Particle statisticsBroader topic: Its stability is a macroscopic consequence of electron exclusion.