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Article overview
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Orbital Parameters for the $250 M_odot$ Eta Carinae Binary System | | Amit Kashi
; Noam Soker
; | | Date: |
14 Aug 2015 | | Abstract: | We show that recent observations of He I and N II lines of Eta Carinae
support an orbital orientation where the secondary star is closest to us at
periastron passages. This conclusion is valid both for the commonly assumed
masses of the two stars, and for the higher stellar masses model where the very
massive evolved primary star mass is $M_1=170 M_odot$ and its hot secondary
star mass is $M_2 = 80 M_odot$. The later model better explains the change in
the orbital period assuming that the ninetieth century Great Eruption was
powered by accretion onto the secondary star. Adopting the commonly used high
eccentricity $e simeq 0.9$ and inclination $i=41^circ$, we obtain a good fit
to newly released Doppler shift observations of He I emission and absorption
lines assuming they are emitted and absorbed in the acceleration zone of the
secondary stellar wind. Our conclusion that the secondary star is in the
foreground at periastron reverses an opposite view presented recently in the
literature. | | Source: | arXiv, 1508.3576 | | Services: | Forum | Review | PDF | Favorites | |
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