Physics
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.182..101p&link_type=abstract
In ESA Ultraviolet Stellar Classification p 101-114 (SEE N82-26119 16-89)
Physics
1
Classifications, Stellar Spectra, Ultraviolet Spectra, Absorption Spectra, Black Body Radiation, Opacity, Parameter Identification, Photosphere, Stellar Temperature, Thermodynamic Equilibrium
Scientific paper
Parameters needed to classify normal stars, parameters which govern parts of the UV spectrum, and ways of distinguishing abnormal stars are reviewed. The use of photospheric spectral features for UV classification is advocated because the major part of the energy radiating from the star originates from the photosphere. Temperature can be obtained by observing longwave flux in the black body curve. Observational criteria can be derived from continua by connecting the UV to the visible spectrum, and by producing pure UV indices. The first method is well suited to A5 to B5 stars. Classification from UV lines should select local thermodynamic equilibrium photospheric lines such that (line center absorption coefficient)/(continuum opacity at the line (Kc)) is small, and Kc not much continuum opacity at 5000 A. Analysis of AP to BP stars shows that temperature and opacity effects are mixed in the UV, prohibiting the use of pure UV indices as temperature indicators.
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