Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982iaus...98..361m&link_type=abstract
In: Be stars; Proceedings of the Symposium, Munich, West Germany, April 6-10, 1981. (A83-10301 01-90) Dordrecht, D. Reidel Publi
Astronomy and Astrophysics
Astronomy
23
B Stars, Stellar Envelopes, Stellar Mass Ejection, Stellar Spectra, Stellar Winds, Ultraviolet Astronomy, Continuous Spectra, Ion Sources, Lyman Spectra, Shell Stars, Spaceborne Astronomy, Spectral Energy Distribution, Spectrum Analysis, Ultraviolet Spectra
Scientific paper
A table summarizing the space experiments in which Be stars have been observed is included. In discussing the continuous energy distribution, it is pointed out that the UV flux deficiency may be explained by the combined effects of line blocking together with hydrogen bound-free absorption, especially in stars with conspicuous shells. Regarding the spectral classification and analysis of ultraviolet spectra, numerous investigations buttress the contention that the physical processes that control the formation of the optical and UV spectra of both Be and B stars of the same spectral type are the same. With regard to the cool circumstellar envelope, it is noted that since the UV flux deficiency seems to increase with increasing envelope density and since among the contributors to absorption at 2100 A are Fe III transitions whose lower levels are metastable, a Be star with a small but significant UV deficit could be called a shell star even though its optical spectrum exhibits no shell lines.
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