The orientation of the η Carinae binary system

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