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\IBVShead{4339}{7 May 1996}

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\centerline{\ft PHOTOGRAPHIC AND CCD PHOTOMETRY OF V350 CEPHEI}
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\begintext

The variability of V350 Cep was discovered by Gyulbudaghian and 
Sarkissian (1977) comparing their photographic observations in 
NGC\,7129 with the Palomar Observatory Sky Survey charts. They found 
the star to be brighter in 1977 with more than 4\fmm\ in B colour 
in comparison with the brightness in 1952. The following photometric 
observations of V350 Cep (Gyulbudaghian and Sarkissian, 1978; 
Hakverdian and Gyulbudaghian 1978; Shevchenko and Yakubov (1989); 
Pogosyants 1991; Semkov 1993) demonstrated changes of brightness, 
which are typical for T Tauri type stars with amplitude of about 
1\fm 5 in B-light. The recent spectral observations of 
V350 Cep made in 1989 (Miranda et al., 1994) confirmed that its 
spectrum is also of a T Tauri type star with a number of emission lines 
and P Cygni profile of H$\alpha$ line.

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\begin{center}
Table 1. Photographic observations of V350 Cep in the period 
December 1992 - August 1994
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\begin{tabular}{|cccc||cccc|}
\hline \raisebox{0pt}[3.0ex][0pt]{}
      
 J.D.    &   U  &   B  &   V  &   J.D.   &   U   &   B   &    V \\
             
 244...  &  mag &   mag &   mag  &   244...  &  mag  &   mag  &   mag\\
\hline  
 8982.2  &  --   &  --  &  15.9   &  9151.4  &  --   &  17.1  &  15.8 \\
 9002.3  &  --  &  17.4  & 16.1  &   9152.4  &  --   &  17.1  &  15.8 \\
 9005.2  &  --   & 17.3  & 16.3  &   9184.5  & 16.3  &  17.1  &  15.6 \\
 9006.2  & 16.8  & 17.0 &  15.8  &   9185.5  & 16.4  &  16.8  &  15.6 \\
 9007.2  &  --  &  17.2  &  --   &   9186.4  &  --   &  16.9  &   -- \\
 9008.2  &  --  &  17.3  &  --   &   9187.5  &  --   &  16.7  &   --\\ 
 9009.2  & 16.8  &  --   &  --   &   9224.4  & 16.3  &  17.0  &   --\\ 
 9029.3  &  --   & 17.1 &  16.2  &   9267.4  & 16.9  &  17.0  &  15.5\\ 
 9036.3   & --   & 17.3  &  --   &   9300.3  &  --   &  16.7  &   -- \\
 9036.6   & --   & 17.4  &  --   &   9354.3   & --   &  16.5  &   --\\
 9038.6  &  --  &  17.0 &   --   &   9452.5  &  --   &  16.4  &   -- \\
 9063.5  &  --  &   --  &  16.1  &   9456.5  & 16.7  &  17.2  &   -- \\
 9067.5  &  --  &  16.7 &  15.7  &   9507.4  &  --   &  17.4  &  16.3 \\
 9096.6  &  --  &  17.3 &  16.3  &   9576.4  &  --   &  17.3  &  15.9 \\ 
 9120.5  &  --  &  17.1 &  16.5  &   9577.3  &  --   &  17.3  &   --  \\
 9149.4  &  --  &   --  &  16.0  &   9579.4  &  --   &  17.3  &  16.7 \\
 9150.4  &  --  &  16.8 &  15.9  &           &       &        &       \\
\hline
\end{tabular}
\end{center}
\vskip 3mm
The present photometric data are a continuation of our investigation 
of V350 Cep which has been carried out since 1984 (Semkov, 1993). The UBV 
photographic observations were made with the 50/70/172 cm Schmidt 
telescope of the National Astronomical Observatory Rozhen (Bulgaria) 
in the period December 1992 - August 1994 (Table 1). The B-light\break
\vfill \eject

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Figure 1. Light curve in B-light of V350 Cep during the period 
July 1987-August 1994 (Semkov 1993 and this paper)
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\centerline{Figure 2. Light curve of V350 Cep from all known observations}
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\centerline{3}
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\noindent
curve only from our observations during 
the period July 1987 - August 1994 is presented in Figure 1. The 
increase in B-light has continued over the period 
December 1992 - August 1994. The BVRI(Kron) CCD photometric 
observations were made with an SBIG ST-6 camera attached to the 
Rozhen 2m RCC telescope (Table 2). The reductions to the standard
BVRI system were made according to Georgiev et al. (1994).
\vskip 3mm

\begin{center}
Table 2. BVRI(Kron) CCD photometry of V350 Cep
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\begin{tabular}{c|cccc}
\hline \raisebox{0pt}[3.0ex][0pt]{}

J.D. (24...)  &    V& B $-$ V &  V $-$ R  & V $-$ I \\           
\hline            
49215.379  &   16.88 &     --  &   0.97 &    2.04 \\
49573.481   &  16.32 &   0.98  &   0.85  &   1.98 \\
50047.399   &  16.14 &   1.05  &   0.98  &   2.10 \\
50048.441  &   16.11 &  1.21   &   0.89  &   2.05 \\  
\hline
\end{tabular}
\end{center}

Using all known observations we composed the light curve in B/pg-band 
of V350 Cep presented in Figure 2. The mean value of the stellar
magnitude for each year from 
all photographic data is taken. In Figure 2 the crosses denote our 
photographic data (Semkov 1993 and this paper), the filled circles: 
photographic data from Pogosyants (1991), the squares: photographic data 
from the Byurakan Schmidt telescope (Gyulbudaghian and Sarkissian 1977, 
1978; Hakverdian and Gyulbudaghian 1978), the filled triangle: visual 
estimation from the Palomar Observatory Sky Survey Prints, the circles: 
the mean photoelectric data from Shevchenko and Yakubov (1989), 
the triangles: our CCD photometric data. From Figure 2 the gradual 
increase of brightness of V350 Cep resembling the FU Ori type star 
V1515 Cyg (Herbig, 1977) can be seen.

This work was partly supported by grants F-340/93 and F-311/93 of the 
National Science Fund of the Ministry of Education, Science and 
Technologies, Bulgaria.
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\beginauthors
\authorsrightcol
     E. H. SEMKOV
     Institute of Astronomy
     Bulgarian Academy of Sciences
     BG-1784 Sofia, Bulgaria
     e-mail: evgeni@carina.wfpa.acad.bg
\endauthors

% Call for macro \references
\references

Georgiev, Ts., Getov, R., Semkov, E., Mutafov, A. Todorova, H., 1994, 
{\it Working group on ``Wide-field imaging", Newsletter}, {\bf 6}, 21

Gyulbudaghian, A. L., Sarkissian, R. A., 1977, {\it Astr. Tsirk.}, No.\,972, 5

Gyulbudaghian, A. L., Sarkissian, R. A., 1978, {\it Astr. Tsirk.}, No.\,982, 4 

Hakverdian, L. G., Gyulbudaghian, A. L., 1978, {\it Astr. Tsirk.}, No.\,1027, 3

Herbig, G. H., 1977, {\it ApJ}, {\bf 217}, 693 

Miranda, L. F., Eiroa C., Fernandes, M., Gomez de Castro A. I., 1994, 
{\it A$\&$A}, {\bf  281}, 864

Pogosyants, A. Yu., 1991, {\it IBVS}, No.\,3624

Semkov, E. H., 1993, {\it IBVS}, No.\,3825 

Shevchenko, V. S., Yakubov, S. D., 1989, {\it Azh}, {\bf 66}, 718

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