COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 574

                                Konkoly Observatory
                                Budapest
                                1971 August 14



  Rosemary Hill Observatory, Department of Physics and
  Astronomy, University or Florida, Gainesville, Florida
              Contribution No. 24

             THE PERIOD OF MW PAVONIS

     The eclipsing binary MW Pavonis (BV 894) was 
observed by the author on five nights during October, 1970,
at the Cerro Tololo Inter-American Observatory. These 
observations were obtained with the 16-inch (40.64 cm),
number 1 telescope and a 1 P 21 photoelectric photometer.
Observations were made in three colors with the use of
standard UBV filters.
     Eggen and Strohmeier in IBVS no. 308 (1968) published
a list of observed times of minima and obtained a period of
0.562979d. After reducing the Cerro Tololo data, however,
this period was found to be incompatible with my observed
times of minima. A compatible set of light elements was
found to be:
          JD 2440862.6117 + 0.79499080d E
                      +-3         +-50


                     [FIGURE 1]


---------------------------------------
       Minima           Epoch      O-C
---------------------------------------
243   8204.542 (s)     -3343.5   -0.018
      8228.465         -3313.5   +0.055
      8263.395         -3269.5   +0.006
      8267.336         -3264.3   -0.028
      8295.222         -3229.5   +0.033
      8314.276         -3205.5   +0.007
      8316.278         -3203.0   +0.022
      8555.549         -2902.0   +0.001
      8641.402         -2794.0   -0.005
      8649.311         -2784.0   -0.046
      8992.401         -2352.5   +0.005
      8994.412         -2350.0   +0.029
      9029.333         -2306.0   -0.030
      9374.375         -1872.0   -0.014
      9376.374         -1869.5   -0.002
      9378.372         -1867.0   +0.008
      9404.252         -1834.5   +0.051
      9654.198         -1520.0   -0.028
      9656.198 (S)     -1517.5   -0.015
244   0120.058 (E)     - 934.0   -0.032
      0120.083         - 934.0   -0.007
      0120.933         - 933.0   +0.048
      0122.888         - 930.5   +0.015
      0124.005         - 929.0   -0.060
      0124.010         - 929.0   -0.055
      0124.016  (E)    - 929.0   -0.049
244   0862.6111 (W)        0.0   -0.0006
      0862.6080            0.0   -0.0037
      0862.6100            0.0   -0.0017
      0863.8065            1.5   +0.0023
      0863.8035            1.5   +0.0042
      0863.8065            1.5   +0.0023
      0864.6035            2.5   +0.0043
      0864.6043            2.5   +0.0051
      0864.6015            2.5   +0.0023
      0870.5585           10.0   -0.0031
      0870.5584           10.0   -0.0032
      0870.5615 (W)       10.0   -0.0001
----------------------------------------

     The light curves of MW Pavonis show a primary
eclipse and a total secondary eclipse of almost equal depth.
In addition, asymmetry is incurred in that the light at
the .25 phase is greater than at the .75 phase. As shown
in the figure, each time of primary minimum has a negative
(O-C) and hence occurs early whereas each time of secondary
minimum has a positive (O-C) and hence occurs late. The
analysis of the light curves is presently underway.



1971 August 5          RICHARD M. WILLIAMON  
                     Rosemary Hill Observatory
                       University of Florida