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\IBVShead{4097}{3 October 1994}                      % Use it with dummy or empty arguments

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\title{Photoelectric minima of eclipsing binaries}

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The following Table gives the photoelecric minima obtained in the years 1991-1993
at the N Copernicus Observatory and Planetarium in Brno (Czech Republic) by means
of the Nasmyth type 0.4-m telescope.

The telescope was used with a single channel photometer and EMI\,6256B 
photomultiplier. Measurements were made in the UBV-system. The integration time 
of one measurement was ten second.

The times of minimum brightness and their standard deviation were determined by 
Kwee-van Woerden's (1956) method. The name of star, the name of the filter, 
heliocentric time of minima, standard deviation, different values of O$-$C
and abbreviations of the observers's name are given in Table 1. The abbreviations
in the column ``Observer'' means:

\noindent DH: Dalibor Han\v{z}l
EN: Eva Neureiterov\'a
PH: Petr H\'ajek
TH: Tom\'a\v{s} Hude\v{c}ek
MN: Martin Navr\'atil
MZ: Miloslav Zejda

\noindent Data for calculating the O$-$C residuals have been taken from the 
following literature:

\noindent O$-$C(I): SAC\,65, Krakow, 1993

\noindent O$-$C(I): GCVS, Moscow, 1985-1987

\vskip 3mm
\centerline{Table 1}
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\small
\hbox to 13cm {
\begin{tabular}{lcccccccl}
\hline
Name& & &JD\,hel&err.&O$-$C(I)& &O$-$C(II)&Obs.\\
\hline
\\
RT And&V&s&48506.3373&0.0016&$-$0.0035& &$-$0.0017&MN\\
 &V& &48600.3639&0.0005&$-$0.0019& &$-$0.0001&MN\\
 &B& &48600.3629&0.0003&$-$0.0029& &$-$0.0011&MN\\
 &U& &48600.3655&0.0004&$-$0.0003& &$-$0.0015&MN\\
 &V& &48646.2751&0.0014&$-$0.0025& &$-$0.0007&MN\\
 &B& &48646.2746&0.0008&$-$0.0030& &$-$0.0012&MN\\
 &U& &48646.2754&0.0004&$-$0.0022& &$-$0.0004&MN\\
DS And& &V&48537.4321&0.0005&+0.0050&=&+0.0050&DH\\
 &B& &48537.4293&0.0007&+0.0023&=&+0.0023&DH\\
RX Ari&V& &48262.3965&0.0002&$-$0.0073& &+0.0097&DH\\
 &B& &48262.3951&0.0005&$-$0.0087& &+0.0083&DH\\
TT Aur&V& &48599.3018&0.0004&+0.0073& &$-$0.0059&DH\\
 &B& &48599.3007&0.0002&+0.0062& &$-$0.0070&DH\\
 &U& &48599.3016&0.0003&+0.0071& &$-$0.0061&DH\\
BF Aur&V&s&48271.3680&0.0004&+0.0052&=&+0.0052&DH/PH\\
 &B&s&48271.3694&0.0003&+0.0066&=&+0.0066&DH/PH\\
 &U&s&48271.3724&0.0011&+0.0096&=&+0.0096&DH/PH\\
VW Cep&V& &48276.4159&0.0005&$-$0.0000& &$-$0.0533&EN\\
 &B& &48276.4144&0.0005&$-$0.0015& &$-$0.0548&EN\\
GS Cep&V&s&48461.4968&0.0012&+0.0006& & &DH\\
 &B&s&48461.4969&0.0020&+0.0007& & &DH\\
 &V& &48500.4957&0.0008&+0.0015& & &DH\\
 &B& &48500.4949&0.0008&+0.0007& & &DH\\
 &V& &48503.4394&0.0011&+0.0019& & &DH\\
 &B& &48503.4397&0.0006&+0.0022& & &DH\\
\hline
\end{tabular}}


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\centerline{2}
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\large
\centerline{Table 1 (cont.)}
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\small
\hbox to 13cm {
\begin{tabular}{lcccccccl}
\hline
Name& & &JD\,hel&err.&O$-$C(I)& &O$-$C(II)&Obs.\\
\hline
\\
GS Cep&V&s&48567.4472&0.0013&$-$0.0060& & DH\\
 &B&s&48567.4484&0.0013&$-$0.0048& & &DH\\
V\,680 Cyg&V& &48445.4665&0.0023&+0.0139& &+0.0433&DH/TH\\
 &B& &48445.4622&0.0008&+0.0096& &+0.0390&DH/TH\\
TT Her&V& &48444.4762&0.0011&$-$0.0038& &+0.0138&DH/TH\\
 &B& &48444.4816&0.0008&$-$0.0016& &+0.0192&DH/TH\\
 &V& &48839.4120&0.0011&+0.0021& &+0.0209&DH\\
 &B& &48839.4124&0.0003&+0.0025& &+0.0213&DH\\
V\,566 Oph&V& &48443.4616&0.0006&+0.0014& &+0.0164&DH/TH\\
 &B& &48443.4623&0.0007&+0.0021& &+0.0170&DH/TH\\
V\,839 Oph&V& &48500.3775&0.0009&+0.0018& &+0.0741&DH\\
 &B& &48500.3772&0.0006&+0.0015& &+0.0738&DH\\
 &V& &48805.4965&0.0002&+0.0048& &+0.0826&DH\\
 &B& &48805.4980&0.0002&+0.0063& &+0.0841&DH\\
FT Ori&V& &48273.2980&0.0003&+0.0021&=&+0.0021&DH/EN\\
 &B& &48273.2975&0.0007&+0.0016&=&+0.0016&DH/EN\\
 &U& &48273.3009&0.0004&+0.0050&=&+0.0050&DH/EN\\
V\,392 Ori&V& &48272.3628&0.0016&+0.0070&=&+0.0070&DH\\
 &B& &48272.3601&0.0008&+0.0043&=&+0.0043&DH\\
GP Peg&B& &48476.4195&0.0007&+0.0008& &$-$0.0177&MZ/DH\\
IU Per&V& &48567.3246&0.0011&$-$0.0176& &+0.0090&DH\\
 &B& &48567.3224&0.0011&$-$0.0198& &+0.0068&DH\\
 &U& &48567.3239&0.0028&$-$0.0183& &+0.0083&DH\\
GR Tau&V& &48619.2975&0.0010&+0.0008& &$-$0.0112&DH\\
 &B& &49619.2971&0.0011&+0.0004& &$-$0.0016&DH\\
BU Vul&V& &48479.4249&0.0009&+0.0038& &+0.0028&DH\\
 &B& &48479.4253&0.0005&+0.0042& &+0.0032&DH\\
\hline
\end{tabular}}
\vskip 5mm

\large

Moments of the secondary minima are labelled by ``s''. As far as the data for
calculating the time of the secondary minima are not given in the above
mentioned literature, we use the phase 0.5 for calculating the O$-$C of the
secondary minima (the secondary minimum is supposed to be in mid-phase between the 
primary ones).

In case the elements in both sources are equal, the O$-$C's are also equal (this
is indicated by the sign ``=''). The GCSV period of GS Cep is definitely wrong,
so corresponding (O$-$C) values are not given.

\vskip 1cm


% Call for macros \authors - \authorsrightcol - \endauthors
\beginauthors
\authorsrightcol
Dalibor HAN\v{Z}L
N. Copernicus Observatory
and Planetarium
Kravi hora
616 00 Brno
Czech Republic
e-mail: HANZL@vm.ics.muni.cz
\endauthors

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\references

GCVS, Moscow, 1985-87

Kwee, K. K. and van Woerden, H., 1956,  {\it Bull. Astron. Inst. Neth.}, 
{\bf 12}, No.\,464

SAC 65, Krakow, 1993

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