COMMISSION 27 OF THE I. A. U.
           INFORMATION BULLETIN ON VARIABLE STARS
                       Number 2553

                                         Konkoly Observatory
                                         Budapest
                                         16 July 1984

                                         HU ISSN 0374-0676



        PHOTOELECTRIC LIGHT CURVES AND PERIOD OF HD 199497


  HD 199497 = BD +19d 4574 was first discovered to be a possible W UMa type
eclipsing binary from its appearance on objective prism plates in 1966 and
then observed photoelectrically by Bond (1976). He used the y filter of the
Stromgren four-colour system and obtained 24 photoelectric observations. These
observations showed that it was a new W UMa type eclipsing system with a
range of 0.15 mag. His light elements are

         JD Hel(Min I) = 2442687.418 + 0.3638d E

  Photoelectric observations of HD 199497 were made with the 48 cm Cassegrain
telescope of the Ege University Observatory on six nights in the summer of
1982. During the observations an unrefrigerated EMI 9781A photomultiplier
tube and B,V filters close to the standard UBV system were used. A total of
199 observational points have been obtained in each colour. BD +19d 4568 was
used as comparison and BD +19d 4576 as check star. No evidence for the 
variability of the comparison star was found.
  We obtained three primary and four secondary minima. The depths of the
minima are nearly equal but the mean depth of the primary minima is slightly

                      Table I
                   The times of minima
Hel.Min.JD.     Min. Filter   O-C       Reference
2442687.418      II   y      0.000      Bond (1976)
  45136.4045     II  B,V     0.0009     This paper
    145.4995     II   "      0.0000        " "
    146.4058      I   "     -0.0033        " "
    149.5053     II   "      0.0036        " "
    150.4082      I   "     -0.0031        " "
    177.3357      I   "      0.0005        " "
    177.5184     II   "      0.0013        " "

greater than that of the secondary. Using all the times of the minima given
in Table I, the new light elements are recalculated by the method of weighted
least squares as follows:

         JD Hel(Min I) = 2445146.4091 + 0.3638368d E
                                  +-9         +-4

 According to the new light elements the primary minimum of Bond (1976) is
a secondary minimum. The light and colour curves are presented in Figure 1
where the individual magnitude differences (variable minus comparison) have
been plotted against the phases. The phases and O-C values in Table I were


                             [FIGURE 1]

       Figure 1   Light and colour curves of the HD 199497


calculated with the new elements. The light curves show that HD 199497 is a
typical W UMa type eclipsing binary. The dispersions exceeding the limits of
observational errors are seen on the light curves.


                    C. SEZER, O. GULMEN, N. GUDUR
                    Ege University Observatory
                    Bornova-Izmir-Turkey

Reference:
Bond, H.E., 1976, I.B.V.S. No. 1214