  We examine a variety of observations that shed light on the orientation of
the semi-major axis of the Eta Carinae massive binary system. Under several
assumptions we study the following observations: The Doppler shifts of some He
I P-Cygni lines that is attributed to the secondary's wind, of one Fe II line
that is attributed to the primary's wind, and of the Paschen emission lines
which are attributed to the shocked primary's wind, are computed in our model
and compared with observations. We compute the hydrogen column density toward
the binary system in our model, and find a good agreement with that deduced
from X-ray observations. We calculate the ionization of surrounding gas blobs
by the radiation of the hotter secondary star, and compare with observations of
a highly excited [Ar III] narrow line. We find that all of these support an
orientation where for most of the time the secondary - the hotter less massive
star - is behind the primary star. The secondary comes closer to the observer
only for a short time near periastron passage, in its highly eccentric (e~0.9)
orbit. Further supporting arguments are also listed, followed by discussion of
some open and complicated issues.
