Ratio of VHE fluxes (integrated between 380 GeV−10 TeV) for any two different points on the orbit characterised by the same distance to the optical star as a function of star temperature and orbital phase. The distribution of scattering electrons was assumed to have a power-law index equal to 2. The dashed-dotted line corresponds to the contour line for a flux ratio of 0.8. Given the relatively large statistical and systematic uncertainties (close to 20%) of the VHE data, in case of a star temperature close to (or higher than)  ~4 × 10⁴ K, the TeV light curve might look symmetric with respect to the periastron passage. However, if the star temperature is lower (e.g.  ~2 × 10⁴ K), the difference in the fluxes for orbital locations with a true anomaly of θ =  ±115° (or θ =  ±2 rad) should be measurable with HESS.