Linked from

The 23 pages that link to Stellar atmosphere, each with the reason it gives.

• Mira variableRelated: Pulsation-driven temperature and opacity changes in this layer alter visible brightness.

• AsteroseismologyRelated: Oscillations become measurable through brightness and velocity changes at the surface.

• Balmer seriesRelated: Absorption in these layers can imprint Balmer lines on stellar spectra.

• OpacityRelated: Opacity determines which atmospheric layers contribute to the spectrum we observe.

• VegaRelated: Vega’s spectrum helps calibrate models of stellar atmospheres.

• Spectral typeRelated: Temperature and composition in this layer shape the spectral features used for classification.

• Stellar metallicityRelated: Atmospheric temperature and pressure shape the spectral lines used to infer abundances.

• O-type starRelated: Its high temperature and ionization state produce the characteristic O-star spectrum.

• Spectral classificationRelated: Temperature, pressure, and composition in the atmosphere produce the patterns used for classification.

• MiraRelated: Pulsation and changing opacity in Mira’s atmosphere shape its observed light curve.

• SubdwarfRelated: Atmospheric composition produces spectral signatures used to recognize metal-poor subdwarfs.

• Yellow supergiantRelated: Atmospheric spectra and winds help characterize these extended, luminous stars.