COMMISSION 27 OF THE I. A, U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 2617

                                   Konkoly Observatory
                                   Budapest
                                   1 November 1984

                                   HU ISSN 0374 - 0676





    PHOTOGRAPHIC PHOTOMETRY OF V 1515 CYGNI IN THE YEARS 1983- 1984


 The results of the photographic photometry of V 1515 Cygni - the third
comfirmed member of fuors (the group of FU Orionis stars) - in the interval
from May 1983 to August 1984 are presented.

                    Table I
--------------------------------------------------
J.D.244..   u    J.D.244..   u    J.D.244..   u
5469.510  15.02  5588.336  15.24  5914.422  15.00
5469.517  15.03  5588.344  15.70  5914.458  15.44
5469.555  15.30  5588.351  15.32  5914.465  15.53
5469.563  15.45  5588.384  15.30  5914.472  15.40
5469.569  15.70  5588.392  15.42  5914.479  15.52
5470.546  15.20  5588.494  15.00  5916.462  15.28
5470.553  15.60  5588.501  15.11  5916.470  15.20
5471.513  15.43  5883.481  15.12  5917.517  15.36
5471.519  15.58  5883.488  15.04  5917.524  15.39
5471.527  15.50  5883.495  15.00  5920.503  15.00
5471.534  15.85  5883.502  15.22  5920.510  15.42
5471.553  15.22  5885.444  15.28  5920.517  15.20
5496.463  15.50  5885.451  15.07  5920.524  15.18
5496.470  16.10  5885.458  15.20  5920.551  15.18
5496.518  15.49  5914.365  15.38  5920.558  15.16
5496.526  15.45  5914.407  15.70  5920.566  14.90 
5496.533  15.68  5914.414  15.00  5920.573  15.42
5587.515  15.13
-------------------------------------------------


We estimated the magnitudes of V 1515 Cygni (see Table I) on 21 multiexposure 
plates (20/28 inch Schmidt telescope, ORWO ZU 21 emulsion, UG2
filter) using the same photometer and standard stars as published in our
previous paper (IVBS, No. 2236, 1982). The multiexposure plates used offer
the possibility to observe  a quick variability of the order of a 10-minute
exposure.
   For the 1983-1984 period the star has kept its brightness, reached at
the end of 1982. which is lower than the brightness of the star at the end of
1979 before its decrease in 1980. During the measurements the brightness of
the star varied with an amplitude of 0.7 mag in the U-band sometimes within
one hour.





                            KATYA P. TSVETKOVA

                        Department of Astronomy and
                        National Astronomical Observatory,
                        Bulgaria Academy of Sciences
                        Sofia - 1184, Lenin Str. 72
                        Bulgaria