The local stellar environment (LSE) - The B emission-line stars

Details The local stellar environment (LSE) - The B emission-line stars The local stellar environment (LSE) - The B emission-line stars

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985msngr..39...17d&link_type=abstract

ESO Messenger (ISSN 0722-6691), March 1985, p. 17-20.

Physics

B Stars, Emission Spectra, Stellar Atmospheres, Stellar Envelopes, Ultraviolet Spectra, Variable Stars, Far Ultraviolet Radiation, Interstellar Matter, Stellar Mass Ejection, Stellar Models

Scientific paper

The LSE of Be stars is characterized in a review of theoretical models and visual and FUV observations, summarizing the reports of Underhill and Doazan (1982) and Thomas (1984). Topics examined include the variable cool LSE proposed on the basis of visible observations only, the variable hot rapidly expanding LSE seen in the FUV, the roles of variable mass flux and/or variable nonradiative energy flux in the variability of Be stars, a tentative empirical decelerated-outflow model accounting for the visible and FUV features, and ongoing observational studies (using IUE, Exosat, and several ESO instruments) of the nonthermal properties of the stellar subatmosphere. Typical C IV line profiles for the Be stars HD 200120 and HD 138749 are shown.

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