COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                       Number 1057

                                 Konkoly Observatory
                                 Budapest
                                 1975 November 4


                     V1057 CYGNI



Photographic observations of this star made on 28 Sept. 1975
with the Uppsala-Kvistaberg Schmidt telescope have given the 
following magnitudes (with probable errors of the order less than
+-0.10 mag.):
         V = 10.45        B = 12.20       U = 13.00
When comparing these magnitudes with those given earlier,
e.g., by Schwartz and Snow (Astrophys.J. 177, L85, 1972),  it
appears that the rate of brightness decrease (Gieseking, Astron.
Astrophys. 31, 117, 1974) has diminished, or even come to an end.
There is, however, an excess decrease in B. Although this maybe
should not be taken too seriously (due to the rapid variations
of about one or two tenths of a magnitude observed during the
general decrease, cf. Gieseking, op. cit.), it might be compared 
to the small decrease in photographic magnitude observed in
FU Orionis around the time when this star developed a G-type,
shell (Wachmann, Zeitschr. f. Astrophys. 35, 74, 1954). Recent
objective-prism spectra unfortunately of a rather poor quality)
suggest that the spectral type has not changed appreciably since
the observations by Schwartz and Snow. There seem, however, to
have appeared absorption features around lambdalambda 9200, 4270 and 4390A,
which may point to the development of a shell. It is hoped that
further observations will settle this issue.





                         G. WELIN
                     Astronomiska Observatoriet
                     S - 751 20 Uppsala, Sweden


                ERRATA-CORRIGE


Correction to IBVS No. 1045
A.J. Nicastro: PHOTOELECTRIC OBSERVATIONS OF DO CEPHEI
The seventh paragraph under the section II. The Flares should
read:
    A few observers have noted that flares occur in a set or
ensemble. Indeed, the present series of observations show this
same feature. We note that 54% of the flares detected occurred
within 5 minutes of another flare, 64% within 15 minutes, 73%
within 30 minutes, and 86% within one hour. This indicates, as
was pointed out by many previous observers, that these events
are associated with some active region on the star.


                                     A.J. NICASTRO


Correction to IBVS No. 1052
P. Tempesti: A SHORT PERIOD LIGHT VARIATION IN NOVA CYGNI 1975
At page 1, lines 18-20 instead of
    "On September 9/10 the amplitudes resulted at least 0.15m
(not all the observations are reported in Fig. 1 on September
14/15 the amplitude seems to be decreased to"
Must be read:
    "On September 9/10 the amplitude resulted at least 0.16m;.
on September 14/15 the amplitude seems to be lowered to...




                        P. TEMPESTI