Disk winds of B[e] supergiants

Details Disk winds of B[e] supergiants Disk winds of B[e] supergiants

1998-12-02

arxiv.org/abs/astro-ph/9812038v1

Astronomy and Astrophysics

Astrophysics

7 pages, LaTeX, 3 ps figures, uses lamuphys.sty from Springer-Verlag, to be published in the proceedings of IAU Coll. 169 "Var

Scientific paper

10.1007/BFb0106353

The class of B[e] supergiants 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, 50-90 km/s, i.e. a factor of about 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.

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