To run the code we need some initial parameters. The initial logarithmic limb-darkening coefficients were taken from the tables given by @Van93 as $x_1$=0.47 and $x_2$=0.48, and are automatically interpolated at each iteration by [phoebe]{}. The effective temperature of the primary star is taken as 6950 K and the ratio of the masses of two components $q$=0.84. We have started with $Mode-2$ meant for detached binary systems, keeping the temperature of the primary and the mass-ratio as fixed parameters. According to the WD code we adjusted the following parameters: $i$ (the orbital inclination), $\Omega_1$ (the potential for the primary), $\Omega_2$ (the potential for the secondary), $T_{\rm eff_2}$ (the effective temperature of the cool star), L$_1$ (the luminosity of the primary), and the zero-epoch offset. The luminosity of the secondary star, L$_2$, was constrained by the model. After a few numbers of runs of the Differential Correction program in $Mode-2$ the sum of residuals squared showed a minimum and the corrections to the adjustable parameters became smaller than their probable errors. The results are presented in Table4. The corresponding computed light curve is shown in Fig.4 as a continuous line.

            Parameters                 V2653Oph             
  ------------------------------- ------------------- -- -- --
              $i^{o}$               81.78$\pm$0.25          
        $T_{\rm eff_1}$ 