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We show that recent observations of He I and N II lines of $\eta$ Carinae mayprovide support for an orbital orientation where the secondary star is closestto us at periastron passages. This conclusion is valid both for the commonlyassumed masses of the two stars, and for the higher stellar masses model wherethe very massive evolved primary star mass is $M_1=170 M_\odot$ and its hotsecondary star mass is $M_2 = 80 M_\odot$. The later model better explains thechange in the orbital period assuming that the ninetieth century Great Eruptionwas powered by accretion onto the secondary star. Adopting the commonly usedhigh eccentricity $e \simeq 0.9$ and inclination $i=41^\circ$, we obtain a goodfit to newly released Doppler shift observations of He I emission andabsorption lines assuming they are emitted and absorbed in the accelerationzone of the secondary stellar wind. Our model in which the secondary star is inthe foreground at periastron is opposite to the view presented recently in theliterature.

Orbital Parameters for the $250 M_\odot$ Eta Carinae Binary System