All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3463fig1.ps}\end{figure}$ Figure 1: Light curves of GSC 00144-03031 in standard V magnitudes. The panels in the upper row show photoelectric data obtained at S. Pedro Mártir Observatory. The panels in the middle row show CCD data obtained at Athens University Observatory. The panels in the lower row are, from left: CCD data obtained at Beersel Hills and SETEC Observatories (JD 2 453 056); CCD data obtained at Athens University Observatory and by MM (JD 2 453 060); CCD data obtained at Beersel Hills and at Athens University Observatories (JD 2 453 067).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3463fig2.ps}\end{figure}$ Figure 2: Power spectra of the GSC 00144-03031 data.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3463fig3.ps}\end{figure}$ Figure 3: Light curves of the two independent terms found in the time series of GSC 00144-03031. The mean magnitude V = 10.198 has been subtracted from the 4722 datapoints.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3463fig4.ps}\end{figure}$ Figure 4: Petersen's diagram for double-mode HADS stars. The upper panel shows the sequences calculated from our models. Solid lines: [Fe/H] = 0.00 dex and three different masses (from 1.80 to 2.00 $M_{\odot }$ ); dashed line: [Fe/H] = -0.50 dex and M = 1.80 $M_{\odot }$ ; dotted line: [Fe/H] = -1.00 dex and M = 1.80 $M_{\odot }$ . The middle panel shows the observed period ratios. The lower panel illustrates the matching between theory and observations: the solid lines are the theoretical sequences calculated for [Fe/H] = 0.00 dex, M = 1.90 $M_{\odot }$ and [Fe/H] = 0.00 dex, M = 2.00 $M_{\odot }$ . The crosses indicate low-metallicity (Pop. II) stars; the open symbols (circles, squares and triangles) indicate Pop. I stars with different masses (1.90, 2.00 and >2.00 $M_{\odot }$ , respectively). The filled circles indicate the Pop. I stars in which the differences in the physical parameters, if any, generate similar period ratio values.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3463fig5.ps}\end{figure}$ Figure 5: Evolutionary tracks calculated for [Fe/H] = 0.00 dex, $d_{\rm over}=0.2$ and four different values for the mass (from 1.70 to 2.00 $M_{\odot }$ ). The filled circle indicates the position of GSC 00144-03031. The open circles, from bottom to top, indicate RV Ari, AI Vel, BP Peg and VX Hya.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3463fig2.ps}\end{figure}$	Figure 2: Power spectra of the GSC 00144-03031 data.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3463fig3.ps}\end{figure}$	Figure 3: Light curves of the two independent terms found in the time series of GSC 00144-03031. The mean magnitude V = 10.198 has been subtracted from the 4722 datapoints.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3463fig5.ps}\end{figure}$	Figure 5: Evolutionary tracks calculated for [Fe/H] = 0.00 dex, $d_{\rm over}=0.2$ and four different values for the mass (from 1.70 to 2.00 $M_{\odot }$ ). The filled circle indicates the position of GSC 00144-03031. The open circles, from bottom to top, indicate RV Ari, AI Vel, BP Peg and VX Hya.
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