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A Survey of Mass Loss from Be and Shell Stars Using Ultraviolet Data from Copernicus

Published online by Cambridge University Press:  14 August 2015

J. M. Marlborough  and
Theodore P. Snow JR.
J. M. Marlborough
Affiliation:
University of Western Ontario, London, Ontario, Canada
Theodore P. Snow JR.
Affiliation:
Princeton University Observatory, Princeton, N.J., U.S.A.

Abstract

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Ultraviolet spectra of intermediate resolution have been obtained with Copernicus of twelve objects classified as Be or shell stars, and an additional 19 dwarfs of spectral classes B0-B4. Some of these spectra show marked asymmetries in certain resonance lines, especially the Si iv doublet at λ 1400 Å, indicating the presence of outflowing material with maximum velocities of nearly 1000 km s−1. Direct evidence for mass loss at these velocities is seen for the first time in dwarf stars as late as B1.5. Later than B0.5, the only survey objects showing this phenomenon are Be stars. Among the stars considered there is a correlation between the presence of mass-loss effects and projected rotational velocity, suggesting that the UV flux from B1-B3 dwarfs is sufficient to drive high-velocity stellar winds only if rotation reduces the effective gravity near the equator. The role of mass-loss in producing the Be star phenomenon and the effects of rotation on mass loss are discussed.

Type
Part III: New Observational Techniques
Information
Symposium - International Astronomical Union , Volume 70: Be and Shell Stars , 1976 , pp. 179 - 189
Copyright
Copyright © Reidel 1976 

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