COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2040

                                 Konkoly Observatory
                                 Budapest
                                 1981 November 12

                                 HU ISSN 0374-0676





     TWO COLOUR PHOTOELECTRIC LIGHT CURVES OF WW Dra




  The RS CVn type eclipsing binary WW Dra (BD +60d 1691 A), the
brighter component of the visual binary ADS 10052, was observed
photoelectrically at the Ege University Observatory from June
30 to December 20, 1980. The observations were made with the
48 cm Cassegrain telescope equipped with an unrefrigerated EMI
9781 A photomultiplier.
  BD +61d 1595 and BD +60d 1682 were used as comparison and
check stars, respectively. The B and V filter which are approximately 
in the standard UBV system, were used and a total of
288 observations in each colour were obtained on 37 nights. All
the differential observations in the sense comparison minus
variable were corrected for atmospheric extinction and the times
of individual observations were reduced to the Sun's centre.
   During the observations only one primary minimum time was
obtained as given below.

  Observed Min I time: Hel.J.D. 24 44 446.3406
  Using the photoelectric times of primary minimum given by
Kizilirmak and Pohl (1974), Mardirossian et al. (1980) and given
above, the following new light elements were computed with the
method of least squares:


       Min.I = Hel.J.D. 24 41 918.4994 + 4.6297444d. E
                                  +-32        +-71


The phases of the observations were computed from light elements
already given above. The differential magnitudes were plotted
against phases and are shown in Figure 1 and 2.


                        [FIGURE 1]

          Figure 1   B light curve of WW Dra

                        [FIGURE 2]

          Figure 2   V light curve of WW Dra


  The analysis of the light curves are in progress and the 
observations of the system will be continued in the coming 
observing season.
  The authors would like to express their gratitude to the
Scientific and Technical Research Council of Turkey for supporting 
this research.





          Z. TUNCA, C. IBANOGLU, M. KURUTAC
          S. EVREN, O. TUMER, A.Y. ERTAN
          Ege University Observatory
          Bornova-Izmir/Turkey