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Co-rotating Circumstellar Clouds around Be Stars
Published online by Cambridge University Press: 26 May 2016
Abstract
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A series of intensive high-resolution spectroscopic observations of 7 Be Stars conducted over 5 years strongly indicates that the source of mass loss in these stars is to be found in magnetic activity coupled with rapid rotation. Magnetic centrifugal acceleration of ionized H and He along open field lines produce the circumstellar disk, while gas trapped in closed magnetic loops are responsible for the periodic variations.
- Type
- Session 1 Observations of Rotating Stars
- Information
- Copyright
- Copyright © Astronomical Society of the Pacific 2004
References
Balona, L.A., Handler, G., Aerts, C., Bozic, H., Guinan, E.F., James, D.J., Kaye, A.B., Shobbrook, R.R., 2001b, MNRAS
327, 1288
Google Scholar
Rivinius, Th., Baade, D., Štefl, S., Maintz, M., 2002, in: Aerts, C., Bedding, T.R., Christensen-Dalsgaard, J. (eds.), Radial and Nonradial Pulsations as Probes of Stellar Physics, ASP Conference Series 259, 240
Google Scholar
Strafella, F., Pezzuto, S., Corciulo, G.G., Bianchini, A., Vittone, A.A., 1998, ApJ
505, 299
Google Scholar
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