Abstract
Extensive IUE observations from 1987–96 have provided compelling evidence for azimuthal asymmetry in the winds of Be stars. Two identified types of wind/FUV flux behavior are briefly discussed. Interpretations based upon both nonradial pulsations and rotation of one or more active regions appear plausible.
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Hahula, M. E., Gies, D. R. (1994): in Pulsation, Rotation, and Mass Loss in Early-Type Stars, ed. L. A. Balona, H. F. Henrichs, J. M. LeContel, (Kluwer, Dordrecht, Boston, London), 100–101
Peters, G. J. (1998): in ESO Workshop on Cyclical Variability in Stellar Winds, ed. L. Kaper & A. Fullerton (Berlin: Springer), 127–133
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© 1999 Springer-Verlag
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Peters, G.J. (1999). Evidence for azimuthal asymmetry in be star winds. In: Wolf, B., Stahl, O., Fullerton, A.W. (eds) Variable and Non-spherical Stellar Winds in Luminous Hot Stars. Lecture Notes in Physics, vol 523. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0106351
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DOI: https://doi.org/10.1007/BFb0106351
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