  We argue that the emission and the absorption components of he N II lines
recently observed in Eta Carinae can originate in the secondary's wind
acceleration zone. We base this claim in part on the presence of these lines in
hot nitrogen rich stars, such as WN 8 stars, and on the expected clumpy nature
of such winds. The envelope of the secondary star in Eta Carinae is expected to
be nitrogen rich due to accretion of few solar masses of the primary luminous
blue variable's nitrogen rich material during the nineteenth century Great
Eruption. Another argument in support of N II lines origin in the acceleration
zone of the secondary wind is the behavior of the emission components. The
emission components of the lines show the same Doppler shift variation as that
of the absorption components. The secondary's-wind origin of the N II lines is
compatible with the binary orientation in which the secondary is closer to us
near periastron passage.
