Other
Scientific paper
Dec 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242.1133b&link_type=abstract
Astrophysical Journal, Part 1, vol. 242, Dec. 15, 1980, p. 1133-1143.
Other
23
Chromosphere, Optical Resonance, Stellar Spectra, Supergiant Stars, Atmospheric Models, Atmospheric Turbulence, Background Radiation, Doppler Effect, Isothermal Processes, Mass Distribution, Opacity, Stellar Temperature, Temperature Distribution, Velocity Distribution, Voigt Effect
Scientific paper
The formation of chromospheric resonance line profiles is examined for the case of the relatively low-density atmospheres appropriate to late-type supergiants. The effects of partial frequency redistribution control the emergent line profiles, to the extent that even an isothermal atmosphere can give rise to apparent emission features. Schematic model chromospheres are used to demonstrate the effects of different velocity fields and temperature-density structures on the line profiles, as a first step toward a clearer understanding of the chromospheric line profiles and why supergiants have broad emission lines (the Wilson-Bappu effect). Neither the Doppler nor the mass column density explanation alone can explain the Wilson-Bappu effect in supergiants, but both theories may play a role.
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