Numerical simulations of wind-equatorial gas interaction in eta Carinae

Abstract

We perform three-dimensional gas-dynamical simulations and show that the asymmetric morphology of the blue and red-shifted components of the outflow at hundreds of astronomical units (AU) from the massive binary system eta Carinae can be accounted for from the collision of the free primary stellar wind with the slowly expanding dense equatorial gas. Owing to the very complicated structure of the century-old equatorial ejecta, that is not fully spatially resolved by observations, we limit ourselves to modelling the equatorial dense gas by one or two dense spherical clouds. Because of that we reproduce the general qualitative properties of the velocity maps, but not the fine details. The fine details of the velocity maps can be matched by simply structuring the dense ejecta in an appropriate way. The blue and red-shifted components are formed in the post-shock flow of the primary wind, on the two sides of the equatorial plane, respectively. The fast wind from the secondary star plays no role in our model, as for most of the orbital period in our model the primary star is closer to us. The dense clouds are observed to be closer to us than the binary system is, and so in our model the primary star faces the dense equatorial ejecta for the majority of the orbital period.

MNRAS, in press

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Cited by in corpus (3)

• Orbital Parameters for the $250M_{\odot }$ Eta Carinae Binary System
• A moderately precise dynamical age for the Homunculus of Eta Carinae based on 13 years of HST imaging
• The orientation of Eta Carinae and the powering mechanism of intermediate luminosity optical transients (ILOTs)