COMMISSION 27 OF THE I. A. U.
           INFORMATION BULLETIN ON VARIABLE STARS
                        Number 1167

                                   Konkoly Observatory
                                   Budapest
                                   1976 August 16


    PHOTOELECTRIC OBSERVATIONS OF HD 184905 AND HD 134793




   Photoelectric observations of the magnetic variable star
HD 184905 in UBV system have been performed by Burke et al. [1]
in 1967-68. In terms of those observations they noticed periodic
light variations and the period was even estimated (P=1.855 days).
In 1970 Morrison et al. [2] observed the star photoelectrically in
four colours (u,v,b,y). They also ascertained the elements of light
variations. The period was estimated as P=2.17 days. On the basis
of presenting all the observations with both periods these authors
came to the conclusion that none of these periods can be given 
preference to.
   In 1968 the magnetic variable HD 189905 was observed photoelectrically 
with the Abastumani Astrophysical Observatory 33cm reflector 
and in 1969 the observations were performed with the 48cm reflector 
(AZT-14A) in three colours (U,B,V).
   Differences between the comparison stars were determined. The
variation of the differences between the comparison stars drew our
attention; either a change in the instrumental system or the variations 
of one of the comparison stars might have explained this fact.
The analysis of our observational material showed no substantial
change in the instrumental system. This gave rise to suspicion 
concerning the variations of HD 184695. Then we considered the 
difference in light between the variable and only the comparison star
HD 184787.
   We made an effort to set out our observations with both periods
and then to compare them. It is clear that the observations in yellow 
and ultraviolet present themselves almost similarly with both
periods. The observations in blue presented with P=1.855 days do not
exhibit any periodic light variations while with p=2.17 days they do
(though the amplitude is small -0.02m). Besides, the light variation
curve in blue is in phase with those constructed for other colours.
In terms of the foregoing we came to the conclusion that our observations 
are presented better with P=2.17 days.

                        [FIGURE 1]

   Figure shows the average curves of light variation for
HD 184905 in UBV light based on p=2.17 days.
   According to the photoelectric observations of Burke et al.
[1] light variations more than 0.015m were not noticed for the magnetic 
variable HD 134793. We have observed this variable photoelectrically 
in 1967-69. The observations show possible variations of
light, 0.08m and 0.05m in ultraviolet, blue and yellow, respectively.





                      N.L. MAGALASHVILI
                      J.I. KUMSISHVILI

                   Abastumani Astrophysical
                        Observatory

References:
1 Burke E., Rolland W., Boy W. 1970, JRAS Can., 65, N 6 [BIBCODE 1970JRASC..64..353B ]
2 Morrison N. and Wolf S. 1971, Publ.A.S.P., 83, N 494 [BIBCODE 1971PASP...83..474M ]