All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{3874fig1.ps} \end{figure}$ Figure 1: The light curve in the R(Cousins) band of S5 0716+714 from February 1997 to March 2003. Vertical bars at the top mark the epochs of our INOV observations.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3874fig2.ps} \end{figure}$ Figure 2: Histogram of the mean R magnitude on the nights of INOV observations.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3874fig3.ps} \end{figure}$ Figure 3: Some examples for INOV of S5 0716+714 observed at different epochs from 2000 to 2003. The solid lines through the data show the linear best-fit used to evaluate $\vert\Delta m/\Delta t\vert$ in each selected interval. Dates of observations are 02-01-2000 ( top left), 12-01-2000 ( top right), 26-02-2001 ( middle left), 03-11-2001 ( middle right), 22-04-2002 ( bottom left), 23-03-2003 ( bottom right).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3874fig4.ps} \end{figure}$ Figure 4: The number distribution of the decreasing values of $\Delta m/\Delta t$ (solid histogram) and of the increasing values (dashed).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3874fig5.ps} \end{figure}$ Figure 5: The frequency distribution of all the variation rates $\vert\Delta m/\Delta t\vert$ (in mag/h) in all the used filters (solid histogram). The exponential law best-fit of this distribution (dotted line). The frequency distribution obtained using only the highest rate ( $\vert\Delta m/\Delta t\vert _{\rm max}$ ) measured each night (dashed histogram).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3874fig6.ps} \end{figure}$ Figure 6: Frequency histogram of the variability time scales $\tau _F$ . The best-fit of the theorical distribution given by Eq. (5) is indicated by the dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3874fig7.ps} \end{figure}$ Figure 7: Plot of $\vert\Delta m/\Delta t\vert$ vs. $\Delta t$ : the magnitude variation rates against the duration of the corresponding time intervals.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3874fig8.ps} \end{figure}$ Figure 8: The variation rates (in mag/h) plotted against the mean R magnitude of the source. Note that the rates above 0.085 mag/h were found only when S5 0716+714 was brighter than R = 13.4, while lower rates were found in any brightness states.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{3874fig9.ps} \end{figure}$ Figure 9: The light curve in the V band observed on 2 January 2000. The upper panel shows photometric data of S5 0716+714 (filled circles) and the magnitude difference of two reference stars (open triangles), shifted by an arbitrary offset; the dashed line is the linear best-fit of a brightening segment. The lower panel shows the difference in S5 0716+714 magnitude with respect to the best-fit line to show the micro-oscillations: in this case the amplitude is $\sim$ 0.05 mag and the duration of a cycle is $\sim$ 3 h.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3874fig10.ps} \end{figure}$ Figure 10: Micro-oscillation of the brightness of S5 0716+714 observed on 2003 February 25. Triangles are the difference between the magnitude of two reference stars with an arbitrary offset. Note the noise increase in the last two hours on both light curves.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3874fig1.ps} \end{figure}$	Figure 1: The light curve in the R(Cousins) band of S5 0716+714 from February 1997 to March 2003. Vertical bars at the top mark the epochs of our INOV observations.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3874fig2.ps} \end{figure}$	Figure 2: Histogram of the mean R magnitude on the nights of INOV observations.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3874fig4.ps} \end{figure}$	Figure 4: The number distribution of the decreasing values of $\Delta m/\Delta t$ (solid histogram) and of the increasing values (dashed).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{3874fig5.ps} \end{figure}$	Figure 5: The frequency distribution of all the variation rates $\vert\Delta m/\Delta t\vert$ (in mag/h) in all the used filters (solid histogram). The exponential law best-fit of this distribution (dotted line). The frequency distribution obtained using only the highest rate ( $\vert\Delta m/\Delta t\vert _{\rm max}$ ) measured each night (dashed histogram).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3874fig6.ps} \end{figure}$	Figure 6: Frequency histogram of the variability time scales $\tau _F$ . The best-fit of the theorical distribution given by Eq. (5) is indicated by the dashed line.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{3874fig7.ps} \end{figure}$	Figure 7: Plot of $\vert\Delta m/\Delta t\vert$ vs. $\Delta t$ : the magnitude variation rates against the duration of the corresponding time intervals.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{3874fig8.ps} \end{figure}$	Figure 8: The variation rates (in mag/h) plotted against the mean R magnitude of the source. Note that the rates above 0.085 mag/h were found only when S5 0716+714 was brighter than R = 13.4, while lower rates were found in any brightness states.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3874fig10.ps} \end{figure}$	Figure 10: Micro-oscillation of the brightness of S5 0716+714 observed on 2003 February 25. Triangles are the difference between the magnitude of two reference stars with an arbitrary offset. Note the noise increase in the last two hours on both light curves.
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