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Stellar Winds and Mass-Loss Rates from Be Stars

Published online by Cambridge University Press:  14 August 2015

Theodore P. Snow Jr.
Theodore P. Snow Jr.*
Affiliation:
University of Colorado at Boulder

Extract

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Resonance-line profiles of SiIII and SiIV lines in 22 B and Be stars have been analyzed in the derivation of mass-loss rates. Of the 19 known Be or shell stars in the sample group, all but one show evidence of winds. It is argued that for stars of spectral type B1.5 and later, SiIII and SiIV are the dominant stages of ionization, and this conclusion, together with theoretical fits to the line profiles, leads to mass-loss rates between 10-11 and 3 × 10-9 for the stars. The rate of mass loss does not correlate simply with stellar parameters, and probably is variable with time. The narrow FeIII shell lines often seen in the ultraviolet spectra of Be stars may arise at low levels in the wind, below the strong acceleration zone. The mass-loss rates from Be stars are apparently insufficient to affect stellar evolution.

Type
VII. UV Observations and Mass Loss
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 377 - 385
Copyright
Copyright © Reidel 1982 

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