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 T$_{ \mathrm{ eff}}$ and gravity at the poles (`g$_{ \mathrm{ eff}}$-effect'); secondly, an equatorial disc with a slow dense wind, produced by the stronger opacities at the equator (`$\kappa$-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 g$_{ \mathrm{ eff}}$-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 $\eta$ Carinae and LBV nebulae are accounted for by the anisotropic ejection from rotating stars.
Categories: astro-ph