COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1196

                              Konkoly Observatory
                              Budapest
                              1976 October 29




   HD 201416 = BD +48d 3289 : A NEW VARIABLE IN CYGNUS


    HD 201416 was used as one of the comparison stars in the
course of photoelectric observations of Nova Cygni 1975 with the
60 cm reflector of the Loiano Astronomical Station (Cacciari et
al. 1976). The observations were made on five nights during a
period ranging from October 1975 to June 1976.
    Having as comparison stars HD 201612 and HD 201599, this
star shows small variations in yellow light with a mean amplitude 
of about 0.02 magnitudes.
    The observations have been corrected for differential 
extinction using both the principal and the second order 
coefficient determined for each night.
    In Table I the mean magnitudes in the UBV Standard System
are given.
   The observed times of minima are presented in Table II; a
least square solution yields the following elements:
           Min = J.D.2442692.557+ 0.248331d E.            (1)
   There is a weak evidence which suggests the existence of
two kinds of equidistant minima, but this result has to be 
confirmed. If it is not true, the period must be halved and the
cycles number doubled (in column 2). In column 3 of Table II 
residuals obtained with the elements (1) are given.
   The light curve in the instrumental system is shown in
Fig. 1. The observations have been ordered using the phase 
computed with (1) and must be read as HD 201599 minus HD 201416;
different symbols label different nights.
   In order to have a better idea of the variation, the 
observations made on J.D.2442692 are shown in Fig. 2.

                     [FIGURE 1]
                     [FIGURE 2]

   A similar variation is not evident in B and U light, and
this fact may only partially be due to a greater scatter of the
data.
  On J.D. 2442956 the mean value of the difference of 
magnitude between the comparison star and the variable is 0.03m
greater than the other ones, thus the data of this night have
been normalized to the mean value of the other nights.
  If the spectral type G5 III determined by Bouigue (1959)
is correct, then the definition of the type of variability 
presents some problems. A reasonable hypothesis might be that the
star is an ellipsoidal variable.
  In order to have a better insight on this star, a spectroscopic 
investigation will be started with the new 152 cm telescope.

         Table I

   Star     alpha    delta    V     B-V    U-B   Sp
           (1900)   (1900)

HD 201416  21h 4.3m  +48 27'  7.78  +1.02  +.61  G5 III
HD 201599  21  5.5   +46 52   7.00  + .39  -.01  F2
HD 201612  21  5.6   +48 20   8.57  - .11  -.25  A0

                 Table    II

        T        E            O-C
2442692.437     -0.5       +0.004d
    692.555      0.        -0.002
    710.428     72.        -0.009
    712.304     79.5       +0.003
    712.424     80.        +0.001
    949.458   1034.5       +0.003
    956.530   1063.        -0.003





                                     C. CACCIARI

                                     F. FUSI PECCI

                                     A. GUARNIERI

                                 Istituto di Astronomia,
                                 Universita di Bologna
                                 Via Zamboni 33, 40126 Bologna,
                                 Italy

References:

Cacciari C., Fusi Pecci F., Guarnieri A., 1976 submitted to
          Soviet Astronomy
Bouigue R., 1959, Toulouse Ann. 27, 47