Plot summarizing the fit of our analytical variability model (Sects. 5.1 and 5.2) to the TESS light curve of ExtEV. The upper panel shows the TESS light curve binned in the orbital phase (black dots) with the best-fit model (blue curve) superimposed. The pink line corresponds to the variability model generated with PHOEBE. Phases A, B, and C from Fig. 12 are shown with vertical dashed lines and labeled. The vertical shaded region marks the range of orbital phases where we expect the secondary component to be partially obscured by the WWC cone. The lower panel shows the residuals from the best fit and their smoothed version (red curve). The zero phase corresponds to the time of periastron passage. More details can be found in the main text.