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[vsnet-alert 972] Var 21 CrB public.

Dear colleagues,
herewith I'm sending you an article about SU UMa nature of Antipin's
variable Var21 CrB submitted to an IBVS. A little bit different version
which contain informations about visual detection of historical outburst
by several observers (G. Poyner, T. Vanmunster, M. Iida, and others -
sorry I forgot the names but they are in the page) is placed on GAMA's web
page (because IBVS don't want visual observation, once again sorry). 
I hope you'll be interested in.
With best regards
					Rudolf
P.S. There are three files in this mail. First one is LaTeX source of main
text, second one (crb.tex) is a light curve and the last one (ibvs.sty) is
IBVS style file. Please enjoy them.

-------
(* var21crb.tex *)
\documentstyle[epsf]{article}
\input ibvs.sty

\begin{document}
\IBVShead{XXXX}{XX XXXX 1997}
\title{Revealing of a new SU UMa type variable star}
\title{Var21 Coronae Borealis}
\begintext


 Var21 Coronae Borealis was discovered and designated by S.V. Antipin
 (Antipin 1996) in 1996. Antipin classified this star as a dwarf nova (U
 Geminorum type) with a
 photographic range of 14.5~-~$<$17.5 magnitudes. Several outbursts were
 observed. Two types of them were found,
 differing by duration. The longer outbursts with duration
 of 15 days or more and the shorter ones with existence of about 10
 days.
This behavior is very common to the SU Ursae Majoris subtype of cataclysmic
 variables. These variable stars are characterized by the
 presence of small-amplitude (semi)periodic modulations in the light curve,
 called {\sl superhumps}.
Even though CCD photomerty was made by M. Iida (Nagamo, Japan) in 1996 and
T. Vanmunster (Landen, Belgium), no superhumps were
detected.

 \medskip

 During the last superoutburst in May 1997, the CCD photometry at {\sl
Nicholas Copernicus Observatory and Planetarium in Brno (Czech Republic)}
was performed on night May 11/12. We used SBIG's CCD camera ST-7 placed in primary
focus of 40cm Newtonian telescope (f=1750mm). For automatic reduction
aperture photometry package MuniPhot (by Filip Hroch, Masaryk
University Brno, using some author's routines), which is based on the well known
DaoPhot II - New generation (P.B. Stetson) was used.


 \begin{center}
 \bigskip
 \input{crb}

\smallskip
  {\sl Fig. 1. Lght curve with three superhump maxima. $V-C$ is
 difference between variable and comparison star.}
 \end{center}



 The observing run started on
 JD 2450580.42 and ended on JD 2450580.59. Total number of exposures
 was 147 (two of them were omitted from the list beacuse of clouds). The star
 was near to 14.6 mag in R-band
 (Kron-Cousins) filter. Each exposure lasted 90 seconds. All images were
 proccesed by standard
 dark-frame and flat-field corrections. The standard deviation of magnitude
 of variable
 star
 was $\sigma=0.05$~mag. The star {\bf GSC 2576.2027} close to Var21 CrB
 position was used as a comparison.

 In the resultant light curve (Fig. 1), three superhump maxima
 were definitely detected. Using Phase Dispersion Minimization (Stelingwerf
 1978) analyzing
 routines written by Taichi Kato (Kyoto University, Japan)
 we obtain value of superhump period as
 $P_{SH}=(0.0743 \pm 0.0006)~day$. This result is well within the range of
 superhump periods of usual SU UMa stars, which lies below the lower limit
 of the {\sl period-gap} (Osaki 1996) of cataclysmic variables, which is
 aproximately from 2 hours to 3 hours.

 \medskip
 Independent CCD photometry performed during the same night by Tonny
 Vanmunster (Vanmunster 1997) has
 confirmed our results.
 So there are good reasons to classify variable star {\bf Var21~CrB}
 as an {\bf UGSU} (U Geminorum, SU UMa subclass) dwarf nova with a range of
 variability (14.5~-~$<$17.5) mag (P) and coordinates:
 $\alpha_{2000}$ = 16\fh 00\fmm 03\fss 7 and
 $\delta_{2000}$ = 33\degr 11\farcmm 15\farcss.

 \medskip
 \noindent
 {\it Acknowledgements}: The author would like to thank Taichi Kato (Kato et al.)
 for valuable
 comments, literature support and providing informations. To all
 administrators of VSNET (Variable Stars Network) home page for their work.
 To Tonny Vanmunster
 for notifying the outburst and independent observation of superhumps
 confirming  our results. Jan Hollan and Zden{\v e}k
 Mikul{\'a}{\v s}ek for valuable comments and manuscript editing. The
 Masaryk University for Internet access.The
 author is grateful to Filip Hroch for aperture photometry software support.


\bigskip

\beginauthors
\authorsrightcol

Rudolf NOV{\'A}K
N. Copernicus Observatory
and Planetarium
Krav\'{\i} hora 2
Brno 616 00, Czech Republic
Internet: rudolfn@physics.muni.cz

\endauthors
\vskip 3mm

\references

Antipin S.V., 1996, {\sl IBVS}, No.\,~{\bf 4343}

Kato T., Nogami D., Baba H., {\it http://vsnet.kusastro.kyoto-u.ac.jp/vsnet}

Stellingwerf R.F., 1978, {\it ApJ 224},~{\bf 224}

Osaki Y., 1996, {\it PASP 108,}~{\bf 39}

Vanmunster T., 1997, private communications and vsnet-alert 896

\end{document}

(*end of var21.crb.tex *)
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% Definition of macro \IBVShead
\def\IBVShead#1#2 {\centerline {\ff COMMISSIONS 27 AND 42 OF THE IAU}
  \centerline {\ff INFORMATION BULLETIN ON VARIABLE STARS}
  \vskip 0.1cm
  \centerline {\rm Number #1}
  \vskip 0.5cm
  \hbox to \textwidth{\hfil
  {\vbox{\hbox{\rm Konkoly Observatory}\hbox{\rm Budapest}
  \hbox{\rm #2}\vskip 0.2cm \hbox{\sl HU ISSN 0374 -- 0676}}}}
  \vskip 0.8cm plus 0cm minus 0.5cm}

% Definition of macro \title
\def\title#1 {\uppercase
  {\centerline {\ft #1} \vskip 1cm plus 0.5cm minus 0.5cm}}

% Definition of macro \begintext
\def\begintext{\large \baselineskip=5mm \noindent}

% Definition of macros \beginauthors - \authorsrightcol - \endauthors
\let\cbb={
\let\cbe=}
\def\beginauthors{\vskip 0cm plus 0cm minus 0cm \hbox to \hsize \cbb
 \hskip 0.5cm \hbox to 6cm \cbb \vbox \cbb \hsize=8cm \obeylines}
\def\authorsrightcol{ \vskip 1mm \cbe \cbe \hskip 2.5cm \hbox to 7cm \cbb \vbox \cbb
 \hsize=7cm \obeylines}
\def\endauthors{ \cbe \cbe \hfil \cbe}

% Definition of macro \references
\def\references {\vskip 1cm plus 0.5cm minus 0.5cm
\noindent References: \hfil
  \vskip 0.3 cm plus 0.1 cm minus 0.1cm
\parindent=-1cm \leftskip 1cm}

% -------------------------------------------------------------------------

(* end of ibvs.sty *)

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