Accretion disk in the binary system V367 Cygni

New photoelectric observations of the interacting binary V367 Cyg were made during two consecutive seasons, 1996 and 1997, using the two-channel photometer at Mt. Suhora Observatory. The BVRI light curves are analyzed and system parameters are derived for two alternative models: with and without an accretion disk. A contact conguration is obtained for the no-disk model. The semidetached model, with a disk around the invisible component gives a better t and, in addition, explains most of the observed features of V367 Cyg. The disk in V367 Cyg has a radius of about Rd =2 3R, almost completely lling the secondary component's Roche lobe. Mass is transferred from the less massive (3:3 M) to the more massive (4:0 M) star at a high rate of 5{7 10 5 M/yr.