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\begin{document}

\IBVShead{5350}{6 December 2002}

\IBVStitle{New Elements for V651 H\lowercase{er} and V1058 O\lowercase{ph}}

\IBVSauth{H\"{a}ussler, K.$^1$; Berthold, T.$^1$$^,$$^2$; Kroll, P.$^2$}

\IBVSinst{Bruno-H.-B\"{u}rgel-Sternwarte, T\"{o}pelstr. 46, D-04746 Hartha, Germany}

\IBVSinst{Sternwarte Sonneberg, Sternwartestr. 32, D-96515 Sonneberg, Germany; email: sternwartehartha@lycos.de, tb@stw.tu-ilmenau.de, pk@stw.tu-ilmenau.de}

\SIMBADobj{V651 Her}
\SIMBADobj{V1058 Oph}


\begintext

\noindent{
{\large {\bf V651 Her}}}

\noindent{
The variability of V651 Her (=S9618 = GSC 962.0663) was announced by \mbox{Hoffmeister}
(DCEP: 13\fmm0 $-$ 14\fmm0) and first elements were derived from Berdnikov et al. (1995):}
$$ \begin{array}{r@{}r@{}l} {\rm Min.~I = HJD~} 2449827.9 & {}
+ 3\fday1745 & {} \times E.\\
\end{array} $$
Recent estimations, made on 244 photographic plates taken with the Sonneberg Observatory 40cm Astrograph,
have yield 8 new times of primary minima (see Table 1).
A least-squares solution including the times of the three deepest measurements from
Berdnikov et al. (1995) yields the following linear ephemeris:
$$ \begin{array}{r@{}r@{}l} {\rm Min.~I = HJD~} 2444373.417 & {}
+ 3\fday174878 & {} \times E.\\
\pm 0.025 & {} \pm 0.000017\\
\end{array} $$
With respect to the magnitudes given in Table 3, the photographic amplitude of \mbox{V651 Her}
was determined to 12\fmm6 $-$ 13\fmm9 (Min. II: 12\fmm9); GCVS type E.
\vskip 6mm

\centerline{Table 1. Minima of V651 Her according to the ephemeris derived in this paper}
\vskip 3mm
\begin{center}
\begin{tabular}{lccrcl}
\hline
Nr   &  HJD  	&Method$^*$	&Epoch	      &$O-C$  & Observer  \\
\hline
1   & 37112.450 &   P   &$   	  -2287.0$&$   -0.020 $ & H\"{a}ussler\\
2   & 38528.508 &   P   &$      -1841.0$&$   +0.041 $ & H\"{a}ussler \\
3   & 39293.497 &   P   &$      -1600.0$&$   -0.115 $ & H\"{a}ussler\\
4   & 44370.400 &   P   &$     -1.0$&$   +0.158 $ & H\"{a}ussler       \\
5   & 44373.426 &   P   &$     0.0$&$   +0.009 $ & H\"{a}ussler \\
6   & 44427.411 &   P   &$     17.0$&$   +0.021 $ & H\"{a}ussler \\
7   & 49132.497 &   P   &$     1499.0$&$   -0.062 $ & H\"{a}ussler       \\
8   & 49475.493 &   P   &$     1607.0$&$   +0.047 $& H\"{a}ussler       \\
9   & 49634.1239&   E   &$     1657.0$&$   -0.0665 $& Berdnikov       \\
10  & 49808.8747&   E   &$     1712.0$&$   +0.0660 $& Berdnikov \\
11  & 49827.7782&   E   &$     1718.0$&$   -0.0797 $& Berdnikov \\

\hline

\end{tabular}
\end{center}
\centerline{$^*$ P denotes photographic plate minima and E photoelectric observations}
\vskip 5mm

\pagebreak
\noindent{
{\large {\bf V1058 Oph}}}

\noindent{
The variability of V1058 Oph (=S9625) was announced by \mbox{Hoffmeister}
(EA, 15\fmm5 $-$ 17\fmm0 photographic, without ephemeris).
A recent investigation, made on 214 photographic plates, has yielded 10 times of
primary minima (see Table 3).}
A least-squares solution has yielded the following linear ephemeris:
$$ \begin{array}{r@{}r@{}l} {\rm Min.~I = HJD~} 2444749.462 & {}+ 5\fday688195 & {} \times E.\\
\pm 0.016 & {} \pm 0.000025\\
\end{array} $$
With respect to the magnitudes given in Table 3, the photographic range of\  \mbox{V1058 Oph}
was determined to 15\fmm8 $-$ 17\fmm3 (Min. II: 16\fmm1); GCVS type E.
\vskip 3mm
Further photometry is urgently needed in the case of V1058 Oph to determine the subtype of variability.
An eccentric orbit cannot be excluded for this system.

\vskip 5mm
\vspace*{2cm}

\centerline{Table 2. Minima of V1058 Oph according to the ephemeris derived in this paper}
\vskip 3mm
\begin{center}
\begin{tabular}{lccrc}
\hline
Nr   &  HJD  	&Method$^*$	&Epoch	      &$O-C$  \\
\hline
1   & 38583.446 &   P   &$   	  -1084.0$&$   -0.013 $ \\
2   & 38640.336 &   P   &$      -1074.0$&$   -0.005 $ \\
3   & 38856.523 &   P   &$      -1036.0$&$   +0.031 $ \\
4   & 44402.422 &   P   &$     -61.0$&$   -0.060 $ \\
5   & 44732.466 &   P   &$     -3.0$&$   +0.068 $ \\
6   & 44749.430 &   P   &$     0.0$&$   -0.032 $ \\
7   & 45056.580 &   P   &$     54.0$&$   -0.045 $  \\
8   & 46592.474 &   P   &$     324.0$&$   +0.037 $  \\
9   & 46649.374 &   P   &$     334.0$&$   +0.055 $  \\
10  & 48088.400 &   P   &$     587.0$&$   -0.033 $ \\

\hline

\end{tabular}
\end{center}
\centerline{$^*$ P denotes photographic plate minima}
\vskip 3mm

\vspace*{2cm}

\centerline{Table 3. Comparison stars}
\vskip 3mm
\begin{center}
\begin{tabular}{ccrcr}
\hline
   &  V651 Her &       &  V1058 Her &        \\
Nr &  GSC/USNO & m$^*$ & GSC/USNO & m$^*$  \\
\hline
1   &  962.0315	&  12\fmm2  & 410.0503	& 15\fmm6\\
2   &  962.2150	&  12\fmm8  & 410.0219	& 16\fmm3\\
3   & 962.1517	&  13\fmm4  & 0900-09216665 & 16\fmm6\\
4   & 962.0335  &  14\fmm0  &            &      \\
\hline

\end{tabular}
\end{center}
\centerline{$^*$ Magnitudes refer to the B values of the USNO-A2.0 catalogue}
\vskip 5mm

\newpage

\IBVSfig{10cm}{5350-f1.eps}{Photographic light curve of V1058 Oph}

This research made use of the SIMBAD data base, operated by the CDS
at Strasbourg, France.


\IBVSedata{5350-t4.txt}
\IBVSedata{5350-t5.txt}

\references

Berdnikov, L.N. et al., 1995, {\it IBVS}, 4213

Hoffmeister, C., 1967, {\it Astron. Nachr.}, {\bf 289}, 205

\end{document}

