  Contrary to recent claims, we argue that the orientation of the massive
binary system Eta Carinae is such that the secondary star is closer to us at
periastron passage, and it is on the far side during most of the time of the
eccentric orbit. The binary orientation we dispute is based on problematic
interpretations of recent observations. Among these observations are the radial
velocity of the absorption component of He I P-Cyg lines, of the He II
$\lambda4686$ emission line, and of the Br$\gamma$ line emitted by clumps close
to the binary system. We also base our orientation on observations of
asymmetric molecular clumps that were recently observed by ALMA around the
binary system, and were claimed to compose a torus with a missing segment. The
orientation has implications for the modeling of the binary interaction during
the nineteenth century Great Eruption (GE) of Eta Carinae that occurred close
to periastron passage. The orientation where the secondary is closer to us at
periastron leads us to suggest that the mass-missing side of the molecular
clumps is a result of accretion onto the secondary star during the periastron
passage when the clumps were ejected, probably during the GE. The secondary
star accreted a few solar masses during the GE and the energy from the
accretion process consists the majority of the GE energy. This in turn
strengthens the more general model according to which many
intermediate-luminosity optical transients (ILOTs) are powered by accretion
onto a secondary star.
