models reproduce relatively well the general appearance of the light curves, the fit at minimum has more scatter than at maximum. It is posible that at minimum the emissivity sources are more complex and our simple model of disk plus spots cannot reproduce so well the overall system emissivity.

Discussion of the light curve models
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Our model indicates a system seen at angle 85and a stellar separation of 65 ${\rm R_{\odot}}$. The stellar temperatures are 4400 $K$ and 14.000 $K$. The stellar masses are 4.83 and 1.06 ${\cal M_{\odot}}$ and surface gravities logg = 3.86 and 2.02. The stellar radii are 4.5 and 16.6 ${\rm R_{\odot}}$. The gainer has a surface temperature indicating a spectral type B6 [@1988BAICz..39..329H], consistent with the B-type spectral types found in DPV gainers. Although we have justified the use of the fixed parameters $T_c$ and $q$, the stellar parameters might be refined when spectroscopic data come to be available.

Significant differences are observed in disk properties when passing from maximum to minimum of the long cycle: the radius increases from 27 to 33 ${\rm R_{\odot}}$, while the temperature at the outer edge remains around 3000-3500 $K$. The vertical thickness at the outer edges increases 