COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1090

                                 Konkoly Observatory
                                 Budapest
                                 1976 February 2


         PHOTOELECTRIC LIGHT CURVES OF AS Cam


     The eclipsing nature of the star AS Cam was announced  by
Strohmeier (1959). Later on the orbital period and photographic
light curve of the system were published by Strohmeier and Knigge
(1960). The system was observed photoelectrically between January
1968 and January 1970 by Hilditch (1972a). In 1969 the light 
elements were calculated by Hilditch using the old photographic and
six photoelectric minima. These elements are
              
          Hel.Min. JD 2440 204.5137+3.4309714d E.
 
     This period is twice of that given by Strohmeier. The light curves
were observed and analyzed by Hilditch in three-colour. The spectroscopic 
orbit of the system was also obtained by Hilditch (1972b).
The system was photoelectrically observed on 19 nights with
the 48 cm Cassegrain telescope of the Ege University Observatory
using an RCA 1P21 photomultiplier and B,V filters.
Two secondary and a primary minimum times were obtained  and
are given in the following table.

--------------------------------------
     Hel.Min.   Min.    O-C   filter
--------------------------------------
 2441547.5273   II     -.2117   B
        .5282   II     -.2108   V
     578.4065   II     -.2112   B,V
     580.3330   I      -.0002   B
        .3338   I      +.0006   V
--------------------------------------

    The light and colour curves are presented in the Figures,
where the magnitude differences between the variable and the 
comparison star (BD+69d317) have been plotted against the phases.
The phases were calculated with the above light elements. The star
varies about 0.625m and 0.595m at the primary, 0.385m and 0.390m at
the secondary minimum in blue and yellow light, respectively. It
is clearly seen that the brightness at the outside eclipses is
variable. The magnitude of these variations are about 0.03m in yellow 
and 0.05m in blue light. On the other hand the epoch of secondary 
minimum is displaced from phase 0.5 to 0.4384. It is difficult
to say anything about the apsidal motion with the available observations.
Further photoelectric minimum times should be obtained for
this purpose.

                       [FIGURE 1]
                       [FIGURE 2]

    This study is a part of Research Project No. 76 supported by
Scientific and Technical Research Council of Turkey.


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



References:

Hilditch, R.W. 1969, The Observatory, 89, 143 [BIBCODE 1969Obs....89..143H ]
Hilditch, R.W. 1972a, Mem.Roy.Astron.Soc 76, 1 [BIBCODE 1972MmRAS..76....1H ]
Hilditch, R.W. 1972b, Pub.A.S.P. 84, 519 [BIBCODE 1969Obs....89..143H ]
Strohmeier, W. 1959, Veroff.Rem.Sternwarte, Bamberg, V, Nr. 3.
Strohmeier, W. and Knigge, R., 1960,Veroff.Rem.Sternw.Bamberg, VII, Nr. 72



            CORRECTION TO IBVS No. 1083

    In the Table for the note on "Close Binaries with H and K
Emission" there is an error in the magnitude of RT Lac. It should
be 9.0 rather than 10.0.          


                            D.M. POPPER