On the nature of the single eclipse per 80d orbit of the H-rich luminous WN star WR22

ABSTRACT WR22 = HD 92740 is a bright (V  = 6.4 mag), intrinsically luminous, double-line WN7h  + O9III-V binary exhibiting one sharp 8 per cent deep eclipse near periastron in its elliptical (e  = 0.6) 80-day orbit, when the WR-star passes in front of the O star, with no secondary eclipse. We apply...

Full description

Saved in:
Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2022-02, Vol.510 (1), p.246-259
Main Authors: Lenoir-Craig, G, Antokhin, I I, Antokhina, E A, St-Louis, N, Moffat, A F J
Format: Article
Language:English
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:ABSTRACT WR22 = HD 92740 is a bright (V  = 6.4 mag), intrinsically luminous, double-line WN7h  + O9III-V binary exhibiting one sharp 8 per cent deep eclipse near periastron in its elliptical (e  = 0.6) 80-day orbit, when the WR-star passes in front of the O star, with no secondary eclipse. We apply two models (L96, A13) to probe the optical space-based light curves from BRITE-Constellation, including three separate, complete eclipses, that show increased (o-c) scatter compared to the rest of the observations outside the eclipses, likely due to O-star light encountering WR wind-clumps. L96 is a simple atmospheric-eclipse model, often applied to close WR + O binaries, where the O-star is considered a point-source. A13 considers a finite-disk O-star and allows for atmospheric, photospheric and reflection components to the eclipse, permitting a better characterization of its shape through a more physically realistic description of the structures for both stars in WR22. Nevertheless, A13 is still susceptible to uncertainties in the luminosity of the O-star before unique values for the orbital inclination and WR mass-loss rate can be estimated. We present solutions for the two extremes of the O-star, O9V and O9III. As photometry alone cannot allow us to discriminate between these, we compared our results to the spectral models found in the literature and determined the correct solution to be O9V. Our best-fitting A13 Model 1 gives i = 83.5 ± 0.4°, with $\dot{M}_{\rm WR} = (1.86 \pm 0.2) \times 10^{-5} \dot{M}_{\odot }/yr$. The flux ratio in the red BRITE band in this model is FO/FWR = 0.064 ± 0.002.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stab3374