An analysis of V616 Mon photoelectric observations during the decline of the 1975 outburst has made it possible to discriminate the brightness variations with the orbital period of Porb = 0d322947 which is close to the present-day value. The period Pb = 7d72 was probably present throughout the time intervals when the brightness was falling down. The brightness decrease results mainly from reradiation of the dropping X-ray flux by the accretion disk and the star. The light curve with Porb is mainly the result of the X ray flux reradiation by the star and of the mutual eclipsing of the star and the disk. Probably, the variations of the orbital light curves with Pb = 7d72 in the early phases of the brightness decrease agree with the model of the accretion disk which is oblique and precessing with this period.
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- Outbursts: Recurrent Novae;
- Periods: Recurrent Novae;
- Recurrent Novae: X-Ray Binaries