COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     Number 1195

                                 Konkoly Observatory
                                 Budapest
                                 1976 October 29



                    V 1057 CYGNI

    Photographic observations of V 1057 Cygni with the Uppsala-
Kvistaberg Schmidt telescope have given the following magnitudes
(with probable errors about +-0.1 mag.):

                  V     B    U
     1976-09-20 10.55 12.15  -
     1976-09-28 10.65 12.2 13.3

Considering the known rapid fluctuations of one or two tenths of
a magnitude, these values do not differ significantly from those
reported one year ago (Welin, IBVS 1057, 1975). The rate of brightness 
decrease must now be definitely less than 0.05 mag. per 100
days, and it seems likely that the decline has stopped altogether.
    Spectra of V1057 Cygni have been obtained in August, 1976,
with the 1.5 m telescope of l'Observatoire de Haute Provence,
equipped with the PEDISCOU spectrograph plus 2-stage RCA image
tube (reciprocal dispersion about 100 Angstrom/mm). These spectra show
a rather strong G-band, which together with, i.a., Ca I 4227
indicates a spectral type of about G0. The hydrogen lines are,
however, too strong for this type. Due to the low resolution of
these image tube plates no conclusive radial velocities could
be measured. The hydrogen and calcium (neutral and ionized) 
absorption lines are generally shifted about 2 Angstrom towards shorter
wavelengths. The K-line has an emission component, apparently
with only a small net radial velocity, situated to the longward
side of the absorption line. That this emission line can be seen
at all suggests that it has grown stronger over the last three
years - it was about as visible on a 20 Angstrom/mm spectrum taken in
August 1973 at Haute Provence.
    In conclusion, V 1057 Cygni has now developed a mixed
spectrum similar to that of FU Orionis (Herbig, Vistas in 
Astronomy, Vol. 8, p. 109, 1966), with a relatively cool, expanding 
shell surrounding the star. The rise of K-line emission
also had its counterpart in the history of FU Orionis.
    The allotment of telescope time at l'Observatoire de Haute-
Provence is gratefully acknowledged, as is a travel grant from
the Swedish Natural Science Research Council. I would also like
to thank Prof. T. Oja and Mr. A. Kinnander for taking the Schmidt
plates.





                           GUNNAR WELIN
                       Astronomiska Observatoriet
                       Box 515, S-751 20 Uppsala,
                             Sweden