COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 1400

                                    Konkoly Observatory
                                    Budapest
                                    1978 March 28




    HD 11285 AND HD 14940: TWO NEW PULSATING VARIABLES

   During the reduction of an observing run (Weiss, 1978) at the
50cm ESO photometric telescope at La Silla (Chile), two further
candidates for pulsation variability have been found among the 
comparison stars. The equipment was the same as described in Weiss
(1977).
HD 11285 (6.8V) is classified as F0 in the HD-catalogue. Figure 1
shows that this star is a short periodic variable with a period of 
approximately 1h50m and an amplitude of about 0.02 mag (increasing
brightness in V and magnitude in (B-V) are plotted in positive 
direction). To demonstrate the photometric accuracy, V magnitudes of
the comparison star HD 11636 are also plotted in this figure. The
phase of (B-V) is similar to that published by Struve (1953). 
Photometric indices in the Stromgren system should be available for
this star to allow for discussion of its absolute magnitude (Breger
and Bregman, 1975).
HD 14940 (6.6V) is also classified as F0 in the HD-catalogue and
shows an extremely small amplitude. Additional observations of this
star should be made to confirm its variability. The present 
observations were made during a night of good photometric stability,
however, with a constant decrease of transparency. HD 14940 was
observed together with HD 15144 and HD 15798. When the V - 
magnitudes for the last two stars were plotted, a systematic trend of
0.009 mag/hr and 0.011 mag/hr, respectively, became evident. In
contrast, the corresponding slope for HD 14940 was 0.0026 mag/hr.
Therefore the V - magnitudes were rectified by subtracting a slope
of 0.001 mag/hr and the result is given in Figure 2.
   The standard deviation for both light curves relative to the
dotted line is 0.0016 mag in both cases. The amplitude of the V-
magnitudes for HD 14940 is about 0.005 mag and the period could be
between 5 and 6 hours. For this star there are no Stromgren indices available either.
Acknowledgements: The author thanks the Gen. Director of ESO,
Dr. Woltjer, for making telescope time available for him as well
as Dr. Muller for his continuous support at La Silla.



Note to I.B.V.S. No. 1364: In Figure 1, increasing magnitudes in
V were plotted in positive direction.





                              WERNER W. WEISS
                         University Observatory and
                         Figl-Observatory f. Astrophys.
                                 Vienna


References:

Breger, M., Bregman, J.N. 1975, ApJ 200, 343 [BIBCODE 1975ApJ...200..343B ]
Struve, O. 1953, PASP 65, 252 [BIBCODE 1953PASP...65..252S ]
Weiss, W.W. 1977, IBVS No. 1364
Weiss, W.W. 1978, Pulsational Stability of Ap-Stars, Observational
             Evidences, in preparation


                         [FIGURE 1]

Figure 1: Variations in V and (B-V) during the night of 25 to 26 Sept. 1977.

                         [FIGURE 2]

Figure 2: V measurements of HD 14940 and HD 15798 during the night of 
10 to 11 Sept. 1977.