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\begin{document}
 
\IBVShead{5962}{6 January 2011}
 
\IBVStitle{Study of the Eccentric-Orbit Binary GSC 03152-01202}

\IBVSauth{Bloomer, R. H$^1$; Della-Rose, D. J.$^2$; Todt, A.$^1$; Zimmerman, J. D.$^1$; Hitefield, S. D.$^1$}
\IBVSinst{King College, USA; rhbloome@king.edu ; atodt@student.king.edu ; jdzimmerman@student.king.edu ; sdhitefield@student.king.edu} %email
\IBVSinst{United States Air Force Academy, USA; Devin.Della-Rose@usafa.edu} %email

\SIMBADobj{GSC 03152-01202} 

\begintext

\IBVSTnam{GSC 03152-01202=UCAC3 84806478}
\IBVSTcoo{20\hr 27\mm 17\fsec27}{+37\deg 56\arcm 26\farcs9}{2000}
\IBVSTobs{U.S. Air Force Academy Observatory, 41 cm and 61 cm Cassegrains}
\IBVSTdet{CCD SBIG ST-2000XM and CCD SBIG STL-11000M}
\IBVSTfil{Green}
\IBVSTdateobs{UT 30 May, 31 May, 20 June, 27 August 2010}
\IBVSTcomp{GSC 3151-1174 = UCAC3 84806456, \hfill\break 20\hr 27\mm 11\fsec2, +37\deg 56\arcm 51\farcs1}
\IBVSTchk{UCAC3 84806530, 20\hr 27\mm 31\fsec2, +37\deg 55\arcm 14\farcs4}
\IBVSTsysn
\IBVSTdata{At the IBVS website (5962-t2.txt)}

\IBVSedata{5962-t2.txt}

\IBVSTtyp{ EA }

\newpage
\IBVSTrem{Bulut et al. (2007) listed GSC 3152-1202 as a candidate for
  eccentric orbits. Otero~et al. (2006) gave light elements stating possible
  confusion of the primary and secondary eclipses and the phase of the
  secondary eclipse to be 0.489. Kozyreva~et~al. (2009) provided new times of 
minimum light for the primary and the secondary eclipses and found the phase of 
the secondary to be 0.5475(5). They proposed a period of apsidal motion of 15 
or 50 years. We were unable to find any other photometric timings of minimum 
light in the literature. Due to this possible rapid motion we measured two 
additional times of primary and two additional times of secondary minimum, and 
we studied a  comparison and a check star that proved stable  (Figure 1).  We 
extracted magnitudes from the flat-fielded images with AIP4Win. Our new times 
of minima are given in Table 1 along with those of Kozyreva et al. We show our 
typical light curves for the two minima in Figure 2 indicating that Otero's 
identification of the primary and secondary to be correct: the depth of the 
primary in green light is 0.$^m$075 deeper than the secondary eclipse. Figure 3 
shows the O-Cs of the primary and secondary eclipses using the current mean 
elements of the two minima. One year after Kozyreva's results, we found the 
phase of the secondary to be 0.5506(3) based on our new elements.  This is 
significantly different from Kozyreva~et al. Rapid rotation of the line of 
apsides seems likely and this star is worthy of additional observations. We 
have computed new light elements for the system using primary eclipse times 
from Kozyreva and this paper: \hbox{Min I = HJD 2455004.4386(1) + 
2.093745(1)$\times$E}. The light elements for the secondary are: Min II = HJD 
245505.5824(1)+2.093799(2)$\times$E.}

\begin{table}[h] 
\centerline{{\bf Table 1.} New Times of Minimum Light for GSC 3152-1202}
\begin{center}
\begin{tabular}{|c|c|c|c|} 
\hline
Type Minimum & HJD Time of Minimum & Uncertainty & Source\\ \hline
I & 2455004.4386 & 0.0002 & 1\\ \hline
II & 2455066.3026 & 0.0003 & 1\\ \hline
II & 2455346.8715 & 0.0005 & 2\\ \hline
I & 2455347.8127 & 0.0006 & 2\\ \hline
II & 2455367.8097 & 0.0003 & 2\\ \hline
I & 2455435.7502 & 0.0002 & 2\\  \hline
\end{tabular}\\
\end{center}
\hspace*{2cm}1 Kozyreva et\,al.\\
\hspace*{2cm}2 This paper\\
\end{table}

\IBVSTack{Zimmerman and Todt acknowledge support of the Appalachian College Association's Ledford grants, and Bloomer acknowledges the support of King College.}

\IBVSfig{8cm}{5962-f1.eps}{The comparison, check and variable stars for this study. The average standard deviation of the differences between the comparison and check stars for the four nights of this work was 0\fmm015 indicating their good stability for photometry.}
\IBVSfigKey{5962-f1.eps}{GSC 03152-01202}{finding chart}

\IBVSfig{7cm}{5962-f2.eps}{Light curves for 20 Jun 10 (secondary) and 27 Aug 10 (primary).  The magnitude and times scales are identical for both curves, and the data points were about five minutes apart.  This shows that the elements of Otero, Kozyreva and this paper correctly identify the eclipses.  All images were checked to be sure no pixels were above 50\% percent saturation.}
\IBVSfigKey{5962-f2.eps}{GSC 03152-01202}{light curve}

\IBVSfig{8cm}{5962-f3.eps}{The O-Cs of the primary times (squares) and the secondary times (diamonds) including the times reported by Kozyreva et al.  These are based on the mean  elements from this study.}
\IBVSfigKey{5962-f3.eps}{GSC 03152-01202}{O-C diagram}

\newpage

\references

Bulut, I. and Demircan, O., 2007, {\it MNRAS}, {\bf 378}, 179

Kozyreva, V.S., Kusakin, A.V., Bagaev, L.A., 2009, {\it IBVS}, 5909

Otero, S.A., Wils, P., Hoogeveen, G, Dubovsky, P.A., 2006, {\it IBVS}, 5681

\endreferences

\IBVSCorrectedVersion{Jan 11 2011}

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