All Figures

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f1.eps} } \end{figure}$ Figure 1: Reduced light variations (upper) and power spectra (lower) of TW Dra obtained for two nights. A sinusoidal curve with a frequency of 18.95 c/d and a semi-amplitude of 5.3 mmag is superimposed in the upper right panel.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f2.eps} } \end{figure}$ Figure 2: Reduced light variations (upper) and power spectra (lower) of RX Hya obtained for two nights. Sinusoidal curves with a frequency of 19.39 c/d and a semi-amplitude of 7.0 mmag are superimposed in the upper panels.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f3.eps} } \end{figure}$ Figure 3: Light variations of the variable star AB Per. The synthetic light curves represented by solid lines in the top panel were constructed using the Wilson-Devinney (1971) method. The lower five panels show residuals after fitting the curves to the data. Sinusoidal curves obtained from the multiple frequency analysis are superimposed on the residuals in four B-band panels.
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In the text

$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{3646_f4.eps} } \end{figure}$ Figure 4: Power spectra of AB Per. Window spectrum is in the top panel. The successive pre-whitening procedure shows three frequencies of f₁ = 0.747 c/d, f₂ = 5.106 c/d and f₃ = 2.624 c/d.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f5.eps} } \end{figure}$ Figure 5: Eclipsing light curves (top), reduced light variations (middle) and power spectra (bottom) of X Tri. We examined only the data during out-of the primary eclipsing phase in order to detect pulsating features of the primary component.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f6.eps} } \end{figure}$ Figure 6: Eclipsing light curves (top), reduced light variations (middle) and power spectra (bottom) of XZ UMa obtained for two nights.
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f7.eps} } \end{figure}$ Figure 7: Reduced light variations (upper) and power spectra (lower) of AC UMa (left) and RW Per (right).
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In the text

$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f1.eps} } \end{figure}$	Figure 1: Reduced light variations (upper) and power spectra (lower) of TW Dra obtained for two nights. A sinusoidal curve with a frequency of 18.95 c/d and a semi-amplitude of 5.3 mmag is superimposed in the upper right panel.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f2.eps} } \end{figure}$	Figure 2: Reduced light variations (upper) and power spectra (lower) of RX Hya obtained for two nights. Sinusoidal curves with a frequency of 19.39 c/d and a semi-amplitude of 7.0 mmag are superimposed in the upper panels.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f3.eps} } \end{figure}$	Figure 3: Light variations of the variable star AB Per. The synthetic light curves represented by solid lines in the top panel were constructed using the Wilson-Devinney (1971) method. The lower five panels show residuals after fitting the curves to the data. Sinusoidal curves obtained from the multiple frequency analysis are superimposed on the residuals in four B-band panels.
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$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{3646_f4.eps} } \end{figure}$	Figure 4: Power spectra of AB Per. Window spectrum is in the top panel. The successive pre-whitening procedure shows three frequencies of f₁ = 0.747 c/d, f₂ = 5.106 c/d and f₃ = 2.624 c/d.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f5.eps} } \end{figure}$	Figure 5: Eclipsing light curves (top), reduced light variations (middle) and power spectra (bottom) of X Tri. We examined only the data during out-of the primary eclipsing phase in order to detect pulsating features of the primary component.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f6.eps} } \end{figure}$	Figure 6: Eclipsing light curves (top), reduced light variations (middle) and power spectra (bottom) of XZ UMa obtained for two nights.
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$\begin{figure} \par {\includegraphics[width=8.8cm,clip]{3646_f7.eps} } \end{figure}$	Figure 7: Reduced light variations (upper) and power spectra (lower) of AC UMa (left) and RW Per (right).
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