COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1166

                                   Konkoly Observatory
                                   Budapest
                                   1976 August 13

       HDE 255930 - A NEWLY-DISCOVERED VARIABLE IN ORION



     In the course of a photoelectric and spectrosropic study of the OB
stars in northern Monoceros (Turner, 1976, Astrophys. J., in press) the star
HDE 255930 (1900 coords: 6h 16.5m, +10d 57') was found to vary by 0.21 magnitude
in V, according to observations on four different nights in November 1974 and
February 1975. No changes in color were detected over this period, and a 
spectrogram of the object led to an MK classification of B2 IV for the star. In order
to learn more about the nature of the variability, additional photoelectric
observations of this star were obtained in March 1976 with the University of
Toronto 61-cm telescope on Cerro Las Campanas, Chile. A catalog of UBV 
observations for this star follows.


 JD 2442000+  V       B-V       U-B

361.798    9.708    +0.145    -0.572
362.646    9.923    +0.101    -0.524
363.650    9.716    +0.109    -0.557
460.559    9.863    +0.108    -0.600
460.631    9.841    +0.103    -0.549
836.611    9.772    +0.122    -0.596
837.597    9.739    +0.117    -0.557
838.528    9.919    +0.099    -0.557
838.530    9.919    +0.101    -0.557
839.535    9.755    +0.105    -0.566
839.536    9.760    +0.100    -0.566
839.618    9.792    +0.085    -0.566
840.533    9.753    +0.104    -0.563
840.535    9.749    +0.112    -0.560
844.546    9.939    +0.100    -0.533
844.548    9.925    +0.109    -0.542
844.591    9.926    +0.126    -0.568
844.592    9.930    +0.111    -0.555
844.618    9.908    +0.104    -0.536
844.620    9.909    +0.118    -0.536
846.550    9.693    +0.102    -0.547
844.551    9.691    +0.112    -0.558


Mean       9.824    +0.109    -0.558




     On the basis of these observations, HDE 255930 appears to be an eclipsing
binary system of the Beta Lyrae type. A period of about 6 days gives the best fit
to the data, although a period of 6 days is also permitted. Further observations
of this newly-discovered variable would clearly be of interest.



                          D.G. TURNER

                          David Dunlap Observatory
                          University of Toronto
                          Richmond Hill, Ontario
                          Canada