Variation of anomalous stages of ionization with spectral type for Be stars

Details Variation of anomalous stages of ionization with spectral type for Be stars Variation of anomalous stages of ionization with spectral type for Be stars

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982iaus...98..387m&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

15

B Stars, Photoionization, Stellar Spectra, Ultraviolet Astronomy, Early Stars, High Resolution, Iue, Line Spectra, Photosphere, Stellar Envelopes

Scientific paper

Results are presented of a preliminary survey of IUE spectra of Be stars covering a wide range of spectral types. For each of 25 UV spectra 23 Be stars obtained six months apart at wavelengths between 1150 and 1950 A, the presence of resonance lines of N V, C IV, and Si IV was studied. The chance of detecting these lines was quantitatively evaluated, and the presence of N V in early Be stars and of both C IV and Si IV in Be stars as cool as B8 demonstrates that at least some Be stars in almost all spectral subdivisions show anomalous stages of ionization in their UV spectra and thus require ionization sources in addition to their photospheric radiation fields. It is suggested that the absence of N V in Be stars cooler than about B2 together with the presence of C IV and Si IV in later types is a real phenomenon and reflects some dependence of the additional ionization source on basic stellar parameters. An attempt is made to determine whether the behavior at B2 and B3 reflects some dependence on v sin i.

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