COMMISSION 27 OF THE I. A. U.
                  INFORMATION BULLETIN ON VARIABLE STARS
                               Number 2484

                                                       Konkoly Observatory
                                                       Budapest 
                                                       1 March 1984

                                                       HU ISSN 0374 - 0676



                     PHOTOELECTRIC OBSERVATION OF THE   
                     FLARE STAR UV Cet IN OCTOBER 1983


   The UV Cet monitoring was carried out on 5/6 October 1983 from 23h 16m
to 01h 23m UT at Crimean Astrophysical Observatory on the 1.25 m Cassegrain
telescope with a one-channel counting photoelectric UBV-photometer. The B-band
close to the Johnson standard system, 0.52 s time integration and 10" diaphragm
were used.
   During the mentioned time interval 5 flares have been recorded, their
characteristics are given in Table I:

a. The universal time of flare maximum, UT_max
b. The flare duration before and after its maximum, t_b and t_a
c. The equivalent duration of the flare, P  
d. The amplitude of the flare, delta m.
  The light curves of the flares observed have been processed previously
by means of a run-medium on three points and are given in Figs. 1-5. The 0.2
mag on 3sigma level is the Limiting magnitude for a flare detection.


                            [FIGURE 1]

                            [FIGURE 2]
                            [FIGURE 3]

                            [FIGURE 4]
                            [FIGURE 5]




                           Table   I
N            UT_max   t_b,min t_a,min   P,min   Delta m
             05.10.83
1            20 58.3     1        4        0.3     0.6
2            21 45.0     7        2        2.7     0.8
3            22 20.5     0.7      7.2      2.0     1.0
4            23 03.2     8.8      0.2      151     4.0
5            23 32.9     0.7      0.3      0.3     0.5

Figures 1 and 5 show light curves with spikes. Figure 3 shows a flare
that may be regarded as a classical one. Figures 2 and 4 show similar curves
but their shapes with instant fading suggest a possible malfunction of our
equipment.



                         I.V. ILYIN
                   Crimean Astrophysical Observatory
                   Nauchny, Crimea, 334413, U.S.S.R.