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The 44 pages that link to Stellar classification, each with the reason it gives.

• H II regionRelated: Hot O- and B-type stars supply the ionizing radiation.

• Apparent magnitudeRelated: Apparent brightness contributes observational data but must be interpreted with distance and color.

• Main sequenceRelated: A main-sequence star receives luminosity class V, distinguishing it from evolved stars of similar temperature.

• Hertzsprung–Russell diagramRelated: Spectral classes provide an alternative scale for the horizontal axis.

• Stellar spectroscopyRelated: Patterns of lines and continua place stars into spectral classes.

• Astronomical spectroscopyRelated: Stellar spectra supply the line patterns used to assign spectral classes.

• Stellar atmosphereRelated: Spectral lines formed in stellar atmospheres help assign stars to spectral classes.

• Stellar massRelated: Mass helps explain why stars occupy different regions of classification diagrams.

• Wolf–Rayet starRelated: Wolf–Rayet subtypes are distinguished chiefly by emission-line patterns and chemical signatures.

• Women in astronomyRelated: Women astronomers made stellar classification a powerful foundation for astrophysics.

• Harvard College ObservatoryRelated: Harvard astronomers developed a spectral sequence that became a standard stellar classification.

• Wien's displacement lawRelated: A star’s spectral peak provides a temperature clue through the displacement relation.

• Spectral energy distributionRelated: Stellar spectral shapes help assign stars to temperature-related classes.

• Williamina FlemingRelated: It describes the systematic task at the center of Fleming’s Harvard work.

• Balmer seriesRelated: Balmer-line strengths help identify temperature ranges and stellar types.

• Kirchhoff's laws of spectroscopyRelated: Absorption-line patterns became a primary basis for distinguishing stellar types.

• Solar luminosityRelated: Luminosities expressed in solar units help distinguish stars along classification diagrams.

• Color indexRelated: Color indices help estimate stellar temperatures and distinguish broad stellar types.

• Optical astronomyRelated: Optical spectra place stars into classes and indicate their temperatures and evolutionary states.

• Hydrogen-alphaRelated: Hydrogen line strengths, including this line, help characterize stellar atmospheres.

• Henry Norris RussellRelated: Spectral classes let Russell relate observed stellar colors to luminosities.

• RigelRelated: Rigel’s spectral type and luminosity class summarize its measured properties.

• AldebaranRelated: Aldebaran’s spectrum places it among cool, evolved stars.

• DenebRelated: Deneb’s spectral type and luminosity class describe its temperature and supergiant status.

• William HugginsRelated: Huggins’s spectral observations helped make stellar composition and type subjects of physical analysis.

• Margaret Lindsay HugginsRelated: Spectral observations of stars contributed to the evidence later used in systematic classification.

• Visible-light astronomyRelated: Visible stellar spectra provide the absorption features used to classify many stars.

• HypergiantRelated: Spectral and luminosity classes help distinguish hypergiants from other massive stars.

• Nancy Grace RomanRelated: Roman’s observations and catalogs contributed to the systematic study of stellar populations.

• UBV photometric systemRelated: UBV colors help distinguish stellar populations and constrain spectral types.

• Epsilon Canis MajorisRelated: Adhara’s B-type spectrum identifies its hot blue-white primary.

• Pi PuppisRelated: Spectra distinguish the cool supergiant from other components.

• Yellow supergiantRelated: Spectral type and luminosity class identify the defining F–G supergiant category.