How strong is the evidence of superionization and large mass outflows in B/Be stars?

Details How strong is the evidence of superionization and large mass outflows in B/Be stars? How strong is the evidence of superionization and large mass outflows in B/Be stars?

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985baicz..36..214h&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 36, July 1985, p. 214-230.

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32

Atmospheric Ionization, B Stars, Stellar Mass Ejection, Stellar Spectra, Carbon, Computational Astrophysics, Nitrogen, Resonance Lines, Silicon

Scientific paper

Consideration is given to the spectroscopic diagnostics of superionization and large mass outflows in B stars according to the UV resonance lines of C IV, SiIV, and N V. The effects of line blending in the vicinity of these lines were estimated by means of a theoretical spectral grid which was computed for main sequence and supergiant model atmospheres in the range of effective temperatures 8000-40,000 K. It is argued that the supergiant spectra may simulate the spectra of Be envelopes well enough to serve as a model. The results are used to demonstrate the observability of shell lines in the Be envelope in the ultraviolet spectrum, even when they are not observable in optical spectra.

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