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Wind Variability in O-Type Stars

Published online by Cambridge University Press:  26 May 2016

H.F. Henrichs ,
L. Kaper  and
J.S. Nichols
H.F. Henrichs
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, and Center for High-Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, Netherlands
L. Kaper
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, and Center for High-Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, Netherlands
J.S. Nichols
Affiliation:
Science Programs, Computer Sciences Corporation, 10000-A Aerospace Rd., Lanham-Seabrook, MD 20706, U.S.A.

Abstract

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The search for the cause of the discrete absorption components (DACs) in P Cygni profiles in UV spectra of O stars continues: pulsation, rotation and magnetic fields are probably all in various degrees important. We highlight some key observations which show that DACs start close to the stellar surface, and emphasize the possible role of localized magnetic fields (which are still to be detected).

Type
7. OB Stellar Winds
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 517 - 529
Copyright
Copyright © Kluwer 1994 

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