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Disk Winds of B[e] Supergiants

Published online by Cambridge University Press:  12 April 2016

Franz-Josef Zickgraf
Franz-Josef Zickgraf*
Affiliation:
Observatoire Astronomique de Strasbourg, 11 rue de l’Université, F-67000 Strasbourg, France

Abstract

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The class of B[e] supegiants is characterized by a two-component stellar wind consisting of a normal hot star wind in the polar zone and a slow and dense disk-like wind in the equatorial region. The properties of the disk wind are discussed using satellite UV spectra of stars seen edge-on, i.e. through the equatorial disk. These observations show that the disk winds are extremely slow, v∞ ≃ 50 ‒ 90 km s−1, i.e. a factor of ~ 10 slower than expected from the spectral types. Optical emission lines provide a further means to study the disk wind. This is discussed for line profiles of forbidden lines formed in the disk.

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. 40 - 48
Copyright
Copyright © Springer-Verlag 1999

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