Hostname: page-component-7479d7b7d-k7p5g Total loading time: 0 Render date: 2024-07-12T13:27:54.987Z Has data issue: false hasContentIssue false
  • English
  • Français

Evidence for Azimuthal Asymmetry in Be Star Winds

Published online by Cambridge University Press:  12 April 2016

Geraldine J. Peters
Geraldine J. Peters*
Affiliation:
Space Sciences Center, University of Southern California, University Park, Los Angeles, CA 90089-1341

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Section I Observations of Non-spherical Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 32 - 35
Copyright
Copyright © Springer-Verlag 1999

References

Hahula, M.E., Gies, D.R. (1994): in Pulsation, Rotation, and Mass Loss in Early-Type Stars, ed. Balona, L.A., Henrichs, H.F., LeContel, J.M., (Kluwer,Dordrecht, Boston, London), 100–101 Google Scholar
Peters, G.J. (1998): in ESO Workshop on Cyclical Variability in Stellar Winds, ed. Kaper, L. & Fullerton, A. (Berlin: Springer), 127–133 Google Scholar