COMMISSION 27 OF THE I. A. U.	
            INFORMATION BULLETIN ON VARIABLE STARS
		         Number 3067


 			 	          Konkoly Observatory
				          Budapest
				          12 August 1987

				          HU ISSN 0374-0676


 OPTICAL BEHAVIOUR OF THE POLAR ST LEONIS MINORIS = CW 1103 + 254 IN THE
  			     SEASON 1986/87

  Using the sequence of comparison stars given in the IBVS No. 2735 the star
was measured on 22 blue-sensitive plates (ORWO-ZU21 + GG13 + BG12) from 14
nights obtained with the 50/70/172 cm Schmidt camera of Sonneberg Observatory
covering the time interval between 27 November 1986 and 23 May 1987. The 
individual observations are listed in Table I.

  Table I

J.D. hel  mB     J.D. hel   mB    J.D. hel   mB
244....          244....          244....

6762.612 15.06   6877.460 15.76   6909.431 15.34
6763.613 14.85   6877.481 15.84   6909.450 16.16
6769.617 14.73   6881.474 16.04   6910.425 16.27
6826.636 15.70   6881.493 16.00   6910.443 15.83
6826.656 15.70   6884.437 15.82   6913.409 16.39
6827.622 15.77   6884.460 16.05   6939.391 16.02
6827.643 16.05   6885.449 15.68   6939.411 16.09
6828.615 15.4 :


  The long time-scale light curve in B is shown in Figure 1.



                        [FIGURE 1]
                        [FIGURE 2]
                        [FIGURE 3]


There a slow decrease of brightness from mB = 14.9m to mB = 16.1m within the
given time interval can be seen. A similar behaviour, which can be explained
as a decrease from the X-ray heated high state to the mean brightness state
could be shown also from the observations of 1986, which are published in the
IBVS No. 2955.

  The observations of the high and the mean brightness state were reduced
to one common epoch by means of the orbital elements given in the IBVS No.
2735. The results are shown in the Figures 2 and 3, where the individual 
observations (smalls dots) and the mean magnitudes (large dots) obtained from
series of the time interval between 1983 and 1985 (IBVS No. 2735) are plotted
against the phase. Both, the individual observations and the mean magnitudes
correspond to the given orbital elements.
  From Figure 2 it can be presumed that the minimum phase of the high state is
displaced to phase ~ 0.5. More observations are needed to make statements
about the behaviour of the orbital light changes in the low state (mB~ 16.7m).



                           W. GOTZ
                     Akademie der Wissenschaften
                     der DDR, Zentralinstitut für
                     Astrophysik, Sternwarte Sonneberg
                     DDR