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We perform three-dimensional gas-dynamical simulations and show that theasymmetric morphology of the blue and red-shifted components of the outflow athundreds of astronomical units (AU) from the massive binary system eta Carinaecan be accounted for from the collision of the free primary stellar wind withthe slowly expanding dense equatorial gas. Owing to the very complicatedstructure of the century-old equatorial ejecta, that is not fully spatiallyresolved by observations, we limit ourselves to modelling the equatorial densegas by one or two dense spherical clouds. Because of that we reproduce thegeneral qualitative properties of the velocity maps, but not the fine details.The fine details of the velocity maps can be matched by simply structuring thedense ejecta in an appropriate way. The blue and red-shifted components areformed in the post-shock flow of the primary wind, on the two sides of theequatorial plane, respectively. The fast wind from the secondary star plays norole in our model, as for most of the orbital period in our model the primarystar is closer to us. The dense clouds are observed to be closer to us than thebinary system is, and so in our model the primary star faces the denseequatorial ejecta for the majority of the orbital period.

Numerical simulations of wind-equatorial gas interaction in eta Carinae