COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                    Number 1558

                                 Konkoly Observatory
                                 Budapest
                                 1979 February 26




    SMALL VARIATIONS IN BRIGHTNESS OF NOVA CYGNI 1975


    Photoelectric observations of Nova Cygni 1975 were carried
out from September 25 till October 7, 1975. During every observational 
night, the observations were going on for several hours
in order to be able to detect any variation in Nova's brightness,
which usually appeared during the transition phase (McLaughlin,
1960). In the case of Nova Cygni 1975 the transition phase 
coincides with the interval from about September the 9th to early
October (Lockwood and Millis, 1976).
    The 63cm Newall refractor of Pentelis Astronomical Station
was used, together with the two beam, multi-mode, nebular stellar
photometer (Goudis and Meaburn, 1973) of the National Observatory
of Athens. The filters used - B and V are in close accordance with
the standard ones. The observations have been reduced using
Hardie's method(1962) and the standard error was found to be +-0.01m
in V and +-0.02m in B.
    Figures 1-3 show the short duration and small amplitude
detected variations in Nova's brightness.





                          PETER ROVITHIS
                     National Observatory of Athens
                         Athens (306) Greece



References:

1. Goudis, C. and Meaburn, J., 1973, Astrophys. and Sp.Sci., 20, 149 [BIBCODE 1973Ap&SS..20..149G ]
2. Hardie, R.H., 1962, Astronomical Techniques, Stars and Stellar
       Systems Vol.II, ed. Hiltner, W.A., The University of
       Chicago Press
3. Lockwood, G.W. and Millis, R.L., 1976, Publ.A.S.P., 88, 235 [BIBCODE 1976PASP...88..235L ]
4. McLaughlin, D.B., Stellar Atmospheres, Kuiper, G.P. and
       Middlehurst, B.M. eds., University of Chicago Press


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