the bright spot temperature is 37% higher than the surrounding disk and 8% at minimum.

We notice that changes in disk parameters, especially disk radius and temperatures of the active regions, might indicate variable mass transfer in the system, as required in the dynamo model proposed by .

\[1\][![Orbital light curves at long cycle maximum and minimum along with the fits provided by the models described in Table2. []{data-label=""}](fits.pdf "fig:"){width="8.5cm"}]{}

Conclusion
==========

-   We find that the eclipsing binary OGLE-BLG-ECL-157529 is a Double Periodic Variable characterized by an orbital period of 2480091 $\pm$ 000044 and a long cycle length decreasing in length and amplitude during 18.5 years of observations.

-   The overall light curves can be understood in terms of a variable accretion disk. The disk is larger and thicker at long cycle minimum and this effect is more pronounced when the long cycle has larger amplitude and longer cycle length.

-   Our models indicate changes in the temperatures of hot spot and bright spot during the long cycle, and also in the position of the bright spot. This, along with the changes in disk radius might indicate variable mass transfer in this system.

We thanks the anonymous referee who 