COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2304

                                    Konkoly Observatory
                                    Budapest
                                    30 March 1983

                                    HU ISSN 0374-0676





       LIGHT VARIATION OF V 1294 Aql IN THE PAST 50 YEARS


  V 1294 Aql (HD 184279, BD + 3d4065, MWC 319, SAO 124788) is a known Be star
with long record of spectroscopic and photometric data. Recently, Horn et al.
(1982) discussed the correlation between the long-term photometric variations
(derived from the photoelectric observations) of the star and the long-term
spectral variations. (See also that paper for detailed bibliography of this
star.)

  In this report we present photometric data derived from visual estimates
on 867 blue-sensitive photographic plates taken in the period 1929 to 1980.
These plates are from the Sonnenberg plate collection and the brightness of
V 1294 Aql was derived by one of us (R.H.).
  The data were reduced and in order to limit the scatter, mean values over
the intervals of 110 days were formed. They are presented together with
available photoelectric measurements and the known history of the shell
development in Figure 1.
  The mean estimated photographic magnitudes of V 1294 Aql were analysed for
possible periods. The overall trend of the brightness was removed and only
the residuals were studied further. Reasonable fit was obtained for periods
of about 2800 - 3000 days, but no strict long-term periodicity was found.
This is also clearly seen from Figure 1.
  We can also derive more information on the correlation between photometric
and spectral variations. Apparently, the actual shell event (which has been
lasting for more than 4000 days now) is accompanied by profound and complex
light variations. It seems that the same type of correlation was observed
at the end of another long-lasting shell from JD 2425000 to JD 2430000.
On the other hand, the relatively short shell period around JD 2432000 passed
without any remarkable light variation.

                         [FIGURE 1]

 Figure 1. Long-term photometric and spectral variation of V 1294 Aql. 
 Photographic
 magnitudes are in the upper panel, while the appearance and disappearance of
 shell lines are on the lowest panel. For comparison, V photoelectric 
 magnitudes are presented in the middle part.





           J. HORN, R. HUDEC and P. KOUBSKY
           Astronomical Institute Czechoslovak
           Academy of Sciences
           251 65 Ondrejov
           Czechoslovakia


Reference:

Horn, J., Bozic, H., Harmanec, P., Koubsky, P., Pavlovski, K., Zdarsky F
  1982, Bull. Astron. Inst. Czechosl. 33, 308 [BIBCODE 1982BAICz..33..308H ]