COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 1124 Konkoly Observatory Budapest 1976 April 6 CONCERNING THE RELATIVE MAGNITUDES OF THE SS CYGNI COMPONENTS Presented here is a small sample of standardized UBV observations of SS Cygni, made with the 24-inch photometric reflector of Lick Observatory when SS Cygni was at minimum. For this sample V_av = 11.66; (B-V)_obs_av.= +0.53 +- 0.05. JD_hel V B-V U-B 2442550.962 11.62+-0.03 0.52+-0.02 -0.70+-0.03 2551.935 11.70 0.50 -0.83 2577.973 11.63 0.41 -0.78 2578.977 11.60 0.53 -1.08 2579.973 11.76 0.71 -1.00 Joy (1956) states that the system consists of a dG5 star and a sdBe companion, and that the absolute magnitudes of the two stars are equal. If one considers a model SS Cygni system consisting of a dG5 star with B-V = +0.70 and a white dwarf companion with B-V= -0.10, at a distance of 270 pc, with a(r) = 1 mag/kpc and R= A_V/E(B-V) = 3(giving E (B-V)= 0.09 mag), then the combined light of the two stars can give an observed (reddened) B-V of +0.53 only if the white dwarf is 1.2 magnitudes fainter in V than the main sequence star. With an absolute visual magnitude of +5.1 for the primary, the combined M_v = +4.8 is consistent with the value derived with the formula M_V = m_V + 5- 5log(r) + A_V, with m_V = 11.66, r = 270 pc, and A_V = 0.27 mag. An uncertainty of +-0.05 mag in the observed B-V results in an uncertainty of +-0.8 mag for the visual magnitude difference between the stars. We may conclude that the hot component of the SS Cygni system is probably fainter in V than its main sequence companion, by about one magnitude. K. KRISCIUNAS 903 Edgewater Drive Naperville, Illinois U.S.A. Reference: Joy, A.H. 1956, Ap. J. 124, 317 [BIBCODE 1956ApJ...124..317J ]