http://arxiv.org/abs/1802.03339
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 passages, and it is on the far side during most of the time of the eccentric orbit. The binary orientation we dispute is based on what we find to be 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, and also a molecular torus with a missing segment that was recently observed by ALMA around the binary system. The orientation has implications to the modeling of the binary interaction during the nineteenth century Great Eruption (GE) of Eta Carinae that occurred close to periastron passages. The orientation where the secondary is closer to us at periastron brings us to suggest that the mass-missing segment of the molecular torus is a result of accretion onto the secondary star during the periastron passage when the torus was 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.
A. Kashi and N. Soker
Mon, 12 Feb 18
49/53
Comments: To be submitted soon. Comments welcome