COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 4081 Konkoly Observatory Budapest 5 September 1994 HU ISSN 0374 - 0676 UBV PHOTOMETRY OF FY Per FY Per was discovered as a variable star by Morgenroth (1936). Some results of investigation of this nova-like cataclysmic variable are published by Shugarov (1980). Recently Sazonov and Shugarov (1993) have discovered that the system's light, changes with a period of 1h33m and an amplitude of 0.15m in B band. FY Per has been observed with the 60 cm telescope and computer controlled photometer of the National Astronomical Observatory Rozhen on several occasions. BD+50d1032 has been used as a comparison star. Each integration was 10 sec through the B filter. In spite of the changes from night to night, the brightness has remained almost constant on the individual nights, and we have not detected any variations on a Lime scale of ~1-2 hours and amplitude larger than 0.035m. Table 1 Date UT N pts B sigma 18 Dec.1993 20h07m- 23h27m 994 12.82m-12.86m 0.012 19 Dec.1993 18 43 - 22 20 1135 12.96-12.99 0.013 21 Dec.1993 22 35 - 22 53 88 13.08-13.10 0.013 Additionally five UBV estimates were obtained: Table 2 JD 2440000+ V B-V U-B 9340.49 12.55 0.29 -0.47 9341.45 12.68 0.30 -0.43 9343.44 12.74 0.35 -0.41 9357.42 12.53 0.30 -0.48 9366.48 12.69 0.35 -0.37 The photometric data here in were reduced using APR software system (Kirov et al., 1992). R. ZAMANOV V. ZAMANOVA NAO Rozhen, Planetarium, POB 136, 4700 Smoljan POB 45, 4700 Smoljan, Bulgaria Bulgaria References: Kirov, N. K., Antov, A. P., Genkov, V. V., 1991, Compt. Rend. Acad. Bulg. Sci., 44, No. 11, 5 Morgenroth, O., 1936, Astron. Nachr., 261, 261 [BIBCODE 1936AN....261..261M ] Sazonov, A. V., Shugarov, S, Yu., 1993, IBVS, No. 3744 Shugarov, S. Yu., 1980, Astron. Tsirk, No. 1199, 3 (in Russian) [BIBCODE 1980ATsir1119....3S ]