Volume 372, Number 1, June II 2001
|Page(s)||L9 - L12|
|Published online||15 June 2001|
The shape of η Carinae and LBV nebulae
Geneva Observatory, 1290 Sauverny, Switzerland e-mail: Andre.Maeder@obs.unige.ch; Vincent.Desjacques@obs.unige.ch
Corresponding author: A. Maeder, Andre.Maeder@obs.unige.ch
Accepted: 11 April 2001
Stellar winds emitted by rotating massive stars may show two main components: firstly bipolar lobes with low density and fast wind, produced by the higher and gravity at the poles ("-effect"); secondly, an equatorial disc with a slow dense wind, produced by the stronger opacities at the equator ("κ-effect"). To see the possible role of this anisotropic wind on the shape of LBV nebulae, we calculate the distribution of the ejected matter in 2 simplified cases: 1) A brief shell ejection. We find that prolate and peanut-shaped hollow nebulae naturally form due to the -effect in rotating stars. 2) A constant wind for a long time. This produces prolate filled nebulae, with a possible strong disc when a bi-stability limit is crossed in the equatorial region. Thus, many features of the η Carinae and LBV nebulae are accounted for by the anisotropic ejection from rotating stars.
Key words: η Carinae / massive stars / LBV stars / mass loss
© ESO, 2001
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