  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.
