  We study the dynamics of continuum driven winds from rotating stars, and
develop an approximate analytical model. We then discuss the evolution of
stellar angular momentum, and show that just above the Eddington limit, the
winds are sufficiently concentrated towards the poles to spin up the star. A
twin-lobe structure of the ejected nebula is seen to be a generic consequence
of critical rotation. We find that if the pressure in such stars is
sufficiently dominated by radiation, an equatorial ejection of mass will occur
during eruptions. These results are then applied to {\eta}-Carinae. We show
that if it began its life with a high enough angular momentum, the present day
wind could have driven the star towards critical rotation, if it is the
dominant mode of mass loss. We find that the shape and size of the Homunculus
nebula, as given by our model, agree with recent observations. Moreover, the
contraction expected due to the sudden increase in luminosity at the onset of
the Great Eruption explains the equatorial "skirt" as well.
