UV observations of mass-loss in Be stars

Details UV observations of mass-loss in Be stars UV observations of mass-loss in Be stars

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.281b.113p&link_type=abstract

In ESA, Proceedings of the Celebratory Symposium on a Decade of UV Astronomy with the IUE Satellite, Volume 2 p 113-116 (SEE N89

Astronomy and Astrophysics

Astronomy

B Stars, Iue, Spaceborne Astronomy, Stellar Mass Ejection, Stellar Winds, Ultraviolet Astronomy, Ultraviolet Spectra, Carbon, Plasma Density, Resonance Lines, Stellar Luminosity

Scientific paper

Mass-loss in 40 Be stars was studied using high resolution IUE spectra. The C IV lambda lambda 1548.2, 1550.8 resonance line profiles are modelled to derive characteristics of the stellar winds. For stars exhibiting evidence of a stellar wind, the ratio v edge/v sec ranges between 0.5 and 2.0, and is a strong function of T eff. The total column density due to discrete components may be less than or = 70 pct of that due to the underlying wind. The product of mass-loss rate and C3(+) ion fraction is clearly a function of luminosity, though the linear slope of this dependence may be shallower than that noted for O stars. As a result of large uncertainties in the C3(+) ion fraction, and the role of absorption due to discrete components, only crude comparisons are possible between mass-loss rates derived from the UV data and IR values.

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