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

WR22 = HD 92740 is a bright (V 6.4 $mag$), intrinsically luminous, double-line WN7h + O9III-V binary exhibiting one sharp 8\% deep eclipse near periastron in its elliptical (e 0.6) 80-day orbit, when the WR-star passes front of O star, with no secondary eclipse. We apply two models (L96, A13) to probe optical space-based light curves from {\em BRITE-Constellation}, including three separate, complete eclipses, that show increased (o-c) scatter compared rest observations outside likely due O-star encountering WR wind-clumps. L96 simple atmospheric-eclipse model, often applied close WR+O binaries, where considered point-source. A13 considers finite-disk and allows for atmospheric, photospheric reflection components eclipse, permitting better characterization shape through more physically realistic description structures both stars WR22. Nevertheless, still susceptible uncertainties luminosity before unique values orbital inclination mass-loss rate can be estimated. present solutions extremes O-star, O9V O9III. As photometry alone cannot allow us discriminate between these, we our results spectral found literature determined correct solution O9V. Our best-fit Model 1 gives $i 83.5 \pm 0.4^{\circ}$, $\dot M_{\rm WR} (1.86 0.2) \times 10^{-5} \dot M_{\odot}/yr$. The flux ratio red BRITE} band this model $F_{\rm O}/F_{\rm 0.064\pm 0.002$.