How strong is the evidence of superionization and large mass outflows in B/Be stars? II - The C IV and SI IV lines in the UV spectra of V 767 Cen, omicron And, Theta CrB, Lambda Eri, and 59 CYG

Details How strong is the evidence of superionization and large mass outflows in B/Be stars? II - The C IV and SI IV lines in the UV spectra of V 767 Cen, omicron And, Theta CrB, Lambda Eri, and 59 CYG How strong is the evidence of superionization and large mass outflows in B/Be stars? II - The C IV and SI IV lines in the UV spectra of V 767 Cen, omicron And, Theta CrB, Lambda Eri, and 59 CYG

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986baicz..37..370h&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 37, Nov. 1986, p. 370-382.

Astronomy and Astrophysics

Astronomy

18

B Stars, Ionization, Stellar Mass Ejection, Stellar Spectra, Ultraviolet Spectra, Photosphere, Resonance Lines, Spectrum Analysis

Scientific paper

The theoretical spectra in the neighborhood of the C IV and Si IV resonance lines have been compared with the published observed spectra of five Be stars, V 767 Cen, omicron And, Theta CrB, Lambda Eri, and 59 Cyg. It is shown that the published determinations of large outflow velocities evidenced by a violet asymmetry of the C IV and Si IV lines, as well as the reports of superionization based on the observations of the C IV and Si IV lines, should be reconsidered in view of considerable line blending effects. In general, it is suggested that many of the puzzling features observed in the UV spectra of B/Be stars may be explained in terms of heavy blending of lines originating in the photospheres and/or subionized, slowly rotating envelopes of the underlying stars.

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