but that decreases its size when time goes by. This should explain why the secondary eclipse is deeper on the beginning. This long-term behavior of the disk is reflected in the secondary eclipse magnitude (Fig.5). When the disk is vertically larger (regarding the orbital plane), it occults a larger fraction of the donor and gainer and the eclipse becomes deeper. However, the deeper secondary eclipses occurs only during long-cycle minima, and this should indicate that the disk size is also modulated by the long cycle, but in a shorter time scale compared with the aforementioned decade-length secular tendency.

We also notice that the disk attains maximum size when the long cycle has larger amplitude and its cycle length is longer, i.e. at the beginning of the time series. We suggest that changes in mass transfer controls the disk size and eventually the brightness of the extra source responsible of the long cycle. This extra source might be a hot spot wind as suggested for the DPV system V393 Scorpii [@2012MNRAS.427..607M] and also for $\beta$ Lyrae . Since we don’t detect changes in the orbital period, the mass transfer in this system should be rather small.

Light curve model
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In 