this subsection we model the light curve in order to test the picture of the variable disk given above. For that we use a theoretical code that solves the inverse problem and that considers a system consistent of a donor star and a gainer star surrounded by an accretion disk, that is both optically and geometrically thick . The disk temperature is the same that the gainer in its inner edge and decreases with a radial profile described by an exponent $a_T$. The model includes a hot spot and a bright spot in the disk, following evidence found in previous observations of algols [@2004AN....325..229R]. These active regions influence the shape of the light curve during the ingress and egress of the eclipses. The model has been described in detail in several papers, so we remit the interested reader to @2013MNRAS.432..799M [@bib:paper6; @2019MNRAS.487.4169M]. We assume a donor temperature $\rm T_{c}$ = 4400K, as derived in the previous section. We also assume synchronous rotation for the donor, as expected for a close binary that rapidly synchronize stellar spins with the orbit due to tidal forces. On the other hand, the gainer might have been spun-up to a high rotation due to nearly 