  I argue that the large scale departure from axisymmetry of the Eta Carinae
nebula can be explained by the binary stars model of Eta Carinae. The companion
diverts the wind blown by the primary star, by accreting from the wind and
possibly by blowing its own collimated fast wind (CFW). The effect of these
processes depends on the orbital separation, hence on the orbital phase of the
eccentric orbit. The variation of the mass outflow from the binary system with
the orbital phase leads to a large-scale departure from axisymmetry along the
equatorial plane, as is observed in Eta Car. I further speculated that such a
companion may have accreted a large fraction of the mass that was expelled in
the Great Eruption of 1850 and the Lesser Eruption of 1890. The accretion
process was likely to form an accretion disk, with the formation of a CFW, or
jets, on the two sides of the accretion disk. The CFW may have played a crucial
role in the formation of the two lobes.
