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We argue that the emission and the absorption components of he N II linesrecently observed in Eta Carinae can originate in the secondary's windacceleration zone. We base this claim in part on the presence of these lines inhot nitrogen rich stars, such as WN 8 stars, and on the expected clumpy natureof such winds. The envelope of the secondary star in Eta Carinae is expected tobe nitrogen rich due to accretion of few solar masses of the primary luminousblue variable's nitrogen rich material during the nineteenth century GreatEruption. Another argument in support of N II lines origin in the accelerationzone of the secondary wind is the behavior of the emission components. Theemission components of the lines show the same Doppler shift variation as thatof the absorption components. The secondary's-wind origin of the N II lines iscompatible with the binary orientation in which the secondary is closer to usnear periastron passage.

The N II Lines in Eta Carinae: A Further Evidence for Mass Transfer During the Nineteenth Century Great Eruption