Analysis of V616 Monocerotis/A 0620-00 brightness variation during the 1975 - 76 outburst.

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 P_orb = 0^d322947 which is close to the present-day value. The period P_b = 7^d72 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 P_orb 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 P_b = 7^d72 in the early phases of the brightness decrease agree with the model of the accretion disk which is oblique and precessing with this period.