COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                      Number 1087

                                 Konkoly Observatory
                                 Budapest
                                 1976 January 25


          PHOTOELECTRIC LIGHT CURVES OF CN And


    The eclipsing binary CN And (BD + 39d0059) was observed 
photoelectrically between July 13 and September 12, 1972 on four nights
with the 48 cm Cassegrain telescope of the Ege University Observatory.
R C A 1P21 photomultiplier and the B, V filters, which are close to
the standard system,were used.
    The first photographic observations of the system were made by
Tsesevich (1956) and the light elements obtained as follow:

      Hel.Min. = JD 2 433 913.386 + 2.2599d . E.

In 1960 Lochel reobserved the star and calculated the light elements
and found as,

      Hel.Min. = JD 2 433 570.465 + 0.46 2798d . E.

    At the same time Lochel classified the system as a W UMa type
close binary.
    Our minimum times do not confirm the light elements of Tsesevich, 
but are in agreement with those of Lochel. However there
is a difference of 56 minutes with the later elements.

                     [FIGURE 1]

            The Table gives our minimum times:
---------------------------------------------------------------
Min.Hel        O-C_I              O-C_II    Color    Min.
---------------------------------------------------------------
2441509.4954 -0.0379            +0.0009       B       II
    509.4930 -0.0403            -0.0015       V       II
    512.5049 -0.0366            +0.0023       B       I
    512.5044 -0.0371            +0.0018       V       I
    567.5761 -0.0383            +0.0005       B       I
    567.5746 -0.0398            -0.0010       V       I
    568.5016 -0.0384            +0.0004       B       I
    568.5012 -0.0388             0.0000       V       I
    577.5282 -0.0364            +0.0024       B       II
    577.5278 -0.0368            +0.0020       V       II
---------------------------------------------------------------
O-C_I according to Lochel (1960)
O-C_II according to our elements (this paper).


We couldn't find any published minimum times for this star
and we have no enough minima for correcting  the light elements.
Therefore one of the times of minimum was chosen as T_0. The
phases of the individual observations were calculated with the
following light elements:

Hel.Min.= JD 2441568.5012+ 0.462798d . E.

The light and color curves are shown in the Figure where the
magnitude differences between the variable and the comparison
star (BD + 39d0051) have been plotted against the phases. The star
varies about 0.565m and 0.550m at the primary minimum, 0.285m and
0.265m at the secondary minimum in blue and yellow, respectively.
Indeed the light curves are similar to a W UMa type as classified
by Lochel.
This study is a part of research project No. 76 supported by
the Scientific and Technical Research Council of Turkey.


                                  S. BOZKURT    O. GULMEN
                                  C. IBANOGLU   N. GUDUR
                                  Ege University Observatory
                                  P.K. 21 Bornova-Izmir, Turkey


References:

Tsesevich, W.  A.C. Kasan, 170, 14. 1956.
Lochel, K.  M.V.S. 457-458. 1960.