Linked from

The 132 pages that link to Stellar evolution, each with the reason it gives.

• Stellar windNarrower topic: Wind-driven mass loss alters a star’s mass, lifetime, and final fate.

• Stellar populationNarrower topic: A population’s observed stars depend on how stellar evolution changes their brightness and lifetimes.

• SupernovaNarrower topic: A star’s evolutionary history determines whether it can become a supernova.

• Supernova remnantNarrower topic: A progenitor’s mass and evolution determine the kind of explosion and remnant it can produce.

• Binary starNarrower topic: Binary interactions can alter both stars' evolutionary paths compared with isolated stars.

• PulsarNarrower topic: A pulsar is one possible endpoint of the evolution of a sufficiently massive star.

• Hertzsprung–Russell diagramNarrower topic: Evolution explains how a star moves between regions of the diagram.

• Planetary nebulaNarrower topic: Planetary nebulae mark a short transition between giant-star evolution and a compact remnant.

• Electron degeneracy pressureNarrower topic: A star's late evolution determines whether its core becomes electron-degenerate.

• Asymptotic giant branchNarrower topic: The asymptotic giant branch is a late stage in this sequence for suitable stars.

• ProtostarNarrower topic: Protostellar growth is the opening stage of a star’s longer evolution.

• Wolf–Rayet starNarrower topic: Wolf–Rayet stars are short-lived stages in the evolution of massive stars.

• Stellar radiusNarrower topic: Expansion and contraction make radius a direct tracer of evolutionary change.

• BetelgeuseNarrower topic: Betelgeuse’s size and variability reflect its advanced evolutionary state.

• SN 1987ANarrower topic: The progenitor’s path to a blue-supergiant state remains central to explaining the event.

• X-ray binaryNarrower topic: A binary’s history determines when its compact object and mass donor form.

• RR Lyrae variableNarrower topic: It explains how old, low-mass stars reach the horizontal branch and become RR Lyrae variables.

• PolarisNarrower topic: Polaris’s changing pulsation period may reflect its evolving position in the instability strip.

• Horizontal branchNarrower topic: The horizontal branch is one short-lived phase in this broader sequence.

• AsteroseismologyNarrower topic: Asteroseismic measurements test models of how stars age and change internally.

• Red dwarfNarrower topic: Red dwarfs evolve unusually slowly because they consume hydrogen at a low rate.

• Red supergiantNarrower topic: Red supergiants are a late stage in the evolution of massive stars.

• Stellar ageNarrower topic: Age dating interprets a star’s present properties as points along an evolutionary track.

• Stellar mass lossNarrower topic: Mass loss became central to explaining how stars change mass and reach their final states.

• S-processNarrower topic: Evolution determines when neutron sources activate and whether synthesized elements reach space.

• StarNarrower topic: A star’s mass determines the broad path it follows from birth to its end.

• Binary black holeNarrower topic: Massive stars can leave black holes that later form binaries.

• Radiative zoneNarrower topic: A star's radiative and convective layers change as its fuel and internal gradients evolve.

• Spectral typeNarrower topic: A star’s spectral type changes as its temperature and atmospheric structure evolve.

• AntaresNarrower topic: Antares's expanded state reflects the late evolutionary phase of a massive star.

• Blue stragglerNarrower topic: A straggler’s position conflicts with the evolutionary stage expected for its cluster’s age.

• Cassiopeia ANarrower topic: The remnant preserves evidence about the final stages of its massive progenitor.

• Circumstellar envelopeNarrower topic: Envelope formation and dispersal are stages in the evolution of many stars.

• Millisecond pulsarNarrower topic: The companion’s evolution determines when and how it transfers mass to the neutron star.

• O-type starNarrower topic: O-type stars evolve rapidly because they burn fuel at exceptionally high rates.

• PleiadesNarrower topic: The cluster’s young age places its member stars near the beginning of their evolution.

• Pair-instability supernovaNarrower topic: The star’s prior evolution determines whether its core enters the pair-instability regime.

• Ring NebulaNarrower topic: The Ring Nebula formed during the late evolution of its progenitor star.

• Tip of the red giant branchNarrower topic: The tip is a brief landmark in the evolution of low-mass stars.

• Henry Norris RussellNarrower topic: Russell interpreted the diagram’s stellar groupings as clues to stars’ life histories.

• Luminous blue variableNarrower topic: Luminous blue variables are a short-lived phase in the evolution of some massive stars.

• 47 TucanaeNarrower topic: 47 Tucanae’s many stars provide snapshots of different stages of stellar evolution.

• Blue supergiantNarrower topic: A blue-supergiant phase is one possible stage in the evolution of a massive star.

• Cat's Eye NebulaNarrower topic: The Cat's Eye formed during the late evolution of its central star.

• Kelvin–Helmholtz mechanismNarrower topic: Contraction-driven luminosity marks an early phase in the broader evolution of stars.

• Red-giant branchNarrower topic: The branch is one stage in the evolution of stars.

• RigelNarrower topic: Rigel’s supergiant state is a brief phase in the evolution of a massive star.

• SubgiantNarrower topic: The subgiant phase is a brief transition in a star’s evolution.

• VY Canis MajorisNarrower topic: VY Canis Majoris is a short-lived, advanced stage in the life of a massive star.

• William Alfred FowlerNarrower topic: Nuclear reaction data constrain how stars burn fuel and change composition.