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\IBVShead{4197}{25 May 1995}

\centerline{\ft BH Cas IS AN ECLIPSING BINARY}
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\begintext

The variability of BH Cas was discovered by Beljawsky (1931) and confirmed by
Kukarkin (1938) who classified it as possibly W~UMa--type with period
$\sim 0.5$ days. Ahnert and Hoffmeister (1943) found no star in the region of
BH Cas with the proposed variation. Metcalfe (1994) published observations
supporting the variability of BH Cas.

In Figure 1, observations of BH Cas obtained in the V--band on the nights of
8~October~1994 (squares) and 19~February~1994 (triangles) are shown. The
comparison star was GSC~03665\,00784 with a measured apparent visual magnitude of 
$13.61 \pm 0.02$.

The light curve confirms that BH Cas is an eclipsing binary of W~UMa--type,
counter to the conclusion of Ahnert and Hoffmeister. The period is $P\sim 0.39$
days, and the HJD epochs of primary and secondary minimum are
$T_{1}=2449767.6661$ and $T_{2}=2449634.7378$ respectively. Observations in the
B-- and R-- bands indicate that (B$-$V)$\approx 0.6$ and (V$-$R)$\approx 0.3$.


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\centerline{Figure 1}
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Future efforts at Steward Observatory will be concentrated on improving the
V--band light curve and determining a more precise period.
Collaboration is especially needed for reconstruction of the B-- and R--band
light curves. Observers at greatly different longitudes than Steward
(L$_{\small w} \simeq 7^{\rm h}~23${\hbox{$.\!\!^{\rm m}$}8) would be most
welcome. For finder charts or additional information, please contact the
undersigned.

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\beginauthors
\authorsrightcol
T.S. METCALFE
Steward Observatory
University of Arizona
Tucson, Arizona, USA
tmetcalf@astro.as.arizona.edu                  %email
\endauthors

\references

Ahnert, P. and  Hoffmeister, C., 1943, {\it KVBB}, {\bf 28}, 4
 
Beljawsky, S., 1931, {\it AN}, {\bf 243}, 115

Kukarkin, B.W., 1938, {\it NNVS}, {\bf 5}, 195

Metcalfe, T.S., 1994, {\it IBVS}, No.\,4038


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