All Figures

$\begin{figure} \par\includegraphics[height=2.3cm,width=6.5cm,clip]{3620fg1a.ps}\... ...*{3mm} \includegraphics[height=2.3cm,width=6.5cm,clip]{3620fg1d.ps} \end{figure}$ Figure 1: From top to bottom: the histogram of the analysed stars for each spectral type as a function of their J magnitude.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig2.ps} \end{figure}$ Figure 2: Weighted average Power Wavelet Transform (PWT) in logarithmic scale of the 50 F-stars analysed. The variance $\sigma ^{2}$ of each entire series is used to weight the average. Continuous line: average PWT of the full time series of data, where a peak at 24 h appears as a consequence of the 22.4% duty cycle of the data. Dashed line: average PWT of the series but removing the zeros from it; the peak at 7 h corresponds to the length of each night of data. Dotted line: average PWT of the series where the mean value of each night's photometry has been substracted from the data. (See text for details.)
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig3.ps} \par\end{figure}$ Figure 3: Mean-weighted average PWTs in logarithmic scale for the F (continuous line), G (dashed line), K (dashed-dotted line), and M (dotted line) analysed stars, above 4.0 $\times 10^{-5}$ Hz , where the data are not filtered.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig4.ps} \end{figure}$ Figure 4: Mean weighted average PWTs in logarithmic scale for the analysed F stars (continuous line) and for the generated power spectrum (dotted line) above $4.0 \times 10^{-5}$ Hz, where the data are not filtered.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig5.ps} \end{figure}$ Figure 5: PWTs in logarithmic scale for 480 days of solar VIRGO data in the blue channel, at the maximum of the solar activity (continuous line) and at the minimum (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig6.ps} \end{figure}$ Figure 6: PWTs in logarithmic scale for 480 days of solar VIRGO data in the three channels (B, G, R) at the maximum of the solar activity.
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In the text

$\begin{figure} \par\includegraphics[height=2.3cm,width=6.5cm,clip]{3620fg1a.ps}\... ...*{3mm} \includegraphics[height=2.3cm,width=6.5cm,clip]{3620fg1d.ps} \end{figure}$	Figure 1: From top to bottom: the histogram of the analysed stars for each spectral type as a function of their J magnitude.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig3.ps} \par\end{figure}$	Figure 3: Mean-weighted average PWTs in logarithmic scale for the F (continuous line), G (dashed line), K (dashed-dotted line), and M (dotted line) analysed stars, above 4.0 $\times 10^{-5}$ Hz , where the data are not filtered.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig4.ps} \end{figure}$	Figure 4: Mean weighted average PWTs in logarithmic scale for the analysed F stars (continuous line) and for the generated power spectrum (dotted line) above $4.0 \times 10^{-5}$ Hz, where the data are not filtered.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig5.ps} \end{figure}$	Figure 5: PWTs in logarithmic scale for 480 days of solar VIRGO data in the blue channel, at the maximum of the solar activity (continuous line) and at the minimum (dotted line).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3620fig6.ps} \end{figure}$	Figure 6: PWTs in logarithmic scale for 480 days of solar VIRGO data in the three channels (B, G, R) at the maximum of the solar activity.
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