Abstract: | With 3D hydrodynamical simulations I show that the asymmetric morphology of the blue and red shifted components of the outflow at hundreds of AU from the massive binary system eta Carinae can be explained by an interaction of the primary stellar wind with the slowly expanding dense equatorial gas. I performed 3D hydrodynamical simulations with the numerical code FLASH, and produced a set of velocity component maps similar to the observed maps. The dense circumstellar gas was ejected in an eruption that occured 115 years ago, and it is concentrated toward us relative to the binary system. Hence, my results strengthen the claim that for most of the time the primary star is closer to us and the secondary is away from us in their highly eccentric orbit around each other. |