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- W4251554440 abstract "Abstract 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." @default.
- W4251554440 created "2022-05-12" @default.
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- W4251554440 date "1999-01-01" @default.
- W4251554440 modified "2023-10-14" @default.
- W4251554440 title "Disk Winds of B[e] Supergiants" @default.
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- W4251554440 doi "https://doi.org/10.1017/s025292110007175x" @default.
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