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\IBVShead{4939}{10 August 2000}

\IBVStitletl{A New High Amplitude Short Period Variable Star}{in Cassiopeia}

\IBVSauth{Antipin, S.V.}

\IBVSinsto{Sternberg Astronomical Institute, 13, Universitetskij Prosp., Moscow 119899, Russia\\ \indent e-mail: antipin@sai.msu.ru}

\IBVSabs{We report discovery and investigation of a new variable star on}
\IBVSabs{Moscow archive plates.}

\SIMBADobj{Antipin V71}
\IBVStyp{high amplitude DSCT or SXPHE}
\IBVSkey{photometry}

\begintext

\IBVSTnam{Var\,71}

\IBVSTcoo{0\hr00\mm52\fsec8}{+62\deg25\arcm15\arcs}{J2000.0}

\IBVSTobs{40-cm astrograph in Crimea}

\IBVSTdet{Photoplate}

\IBVSfig{7.6cm}{4939-f1.ps}{The finding chart and the comparison stars.}

\IBVSfig{7.6cm}{4939-f2.ps}{The phased light curve. Uncertain estimates are shown as open circles.}

\IBVSTfil{None}

\IBVSTcomp{See Fig.~1}

\IBVSTchk{None}

\IBVSTsys{$B_{pg}$}{$B_{pg}$-band standard sequence in NGC 7790
(Pedreros et al., 1984)}

\IBVSTdata{Upon request}

\IBVSTtyp{High amplitude DSCT or SXPHE}

\IBVSTrem{
The star was estimated on 856 plates taken from JD\,2432853 to 2449633.
Variability with a very short period, $P=0\fday 0865524$, was found.
The exposure time of most plates from Moscow collection is 45 minutes
(0\fday 03125). So one plate accumulated the light of one third part of
the period. The situation results in the following inaccuracies. Firstly,
the amplitude of variability taken from the photographic phased light curve
is noticeably understated. The range of variability in Figure~2 does not
represent the real one. Secondly, the shape of the phased light curve is
distorted, it looks more symmetric. The apparent ${\rm max-min}$ value is higher than the
real one. The zero phase ${\rm HJD}_0=2441186.463$, that was used to construct
Figure~2, is not the real moment of maximum brightness. The maximum happened
slightly earlier than we see from the photographic observations.
As to classification, the variable is a new high amplitude (${\rm amp}_B>0\fmm 45$)
short period pulsator of DSCT or SXPHE type. It is necessary to note that the
period of the variation is stable for the investigated time interval.
Further CCD observations are strongly encouraged to determine the real amplitude
of variability, light curve shape and time of maximum brightness of the
star.}

\IBVSTack{
This study was supported in part by the Russian Foundation
for Basic Research and the Council of the Program for the Support of
Leading Scientific Schools through grants Nos.\ 99-02-16333 and 00-15-96627.}

\reference

Pedreros, M., Madore, B.F., Freedman, W.L., 1984, {\it ApJ}, {\bf 286}, 563

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