All Figures

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{b3460f1.ps} \end{figure}$ Figure 1: Light curve of the Sun observed with Yohkoh with the Al ( top panel) and AlMg filter ( bottom panel). Time is measured starting from January 1st 1992. Note the minimum and the maximum observed on 1996 and 2000, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{b3460f2.ps} \end{figure}$ Figure 2: Intensity cumulative distribution observed on the Sun with the AlMg filter during the cycle (solid line). Dashed lines are the distributions observed in individual years. Thin dotted line is the log-normal distribution with the same standard deviation than that of the solar distribution observed during the cycle.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f3.ps} \end{figure}$ Figure 3: Percentiles of the distributions obtained simulating pairs of solar AlMg observations as function of separation time. The marked solid line indicates the median, while the other lines correspond to the 10, 25, 75, and 90% percentiles.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{b3460f4.ps}\hspace*{4mm} \includegraphics[width=7.8cm,clip]{b3460f4b.ps} \end{figure}$ Figure 4: Left panel: cumulative distribution of the amplitude variations obtained from the AlMg filter solar X-ray observations, when observed at different time scales. The legend in the figure indicates the explored time scales. The stepped curve is the cumulative distribution of the amplitude variations obtained for the nearby F7-K2 main sequence stars (109 data points) Right panel: same as in left panel, but with the cumulative distribution of the amplitude variations obtained for the nearby stars observed with time distance greater than 3 days alone (46 data points, stepped distribution).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f5.ps} \end{figure}$ Figure 5: The dots indicate the amplitude of X-ray variations observed in solar-type stars of Marino et al. (2002) in the band 0.7-2.4 keV vs. time scale. Arrows mark the median values of stars observed with time separation of the same order. The solid line marks the median value of the amplitude variations obtained from the AlMg Yohkoh observations of the Sun of Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f6.ps} \end{figure}$ Figure 6: Residuals of the stellar amplitude variations from the solar median of Fig. 3 for stars in our sample versus time scale. Empty points mark stars with $\overline {L}_x <10^{28}$ erg/s while filled points are stars with $\overline {L}_x >10^{28}$ erg/s.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{b3460f1.ps} \end{figure}$	Figure 1: Light curve of the Sun observed with Yohkoh with the Al ( top panel) and AlMg filter ( bottom panel). Time is measured starting from January 1st 1992. Note the minimum and the maximum observed on 1996 and 2000, respectively.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{b3460f2.ps} \end{figure}$	Figure 2: Intensity cumulative distribution observed on the Sun with the AlMg filter during the cycle (solid line). Dashed lines are the distributions observed in individual years. Thin dotted line is the log-normal distribution with the same standard deviation than that of the solar distribution observed during the cycle.
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$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f3.ps} \end{figure}$	Figure 3: Percentiles of the distributions obtained simulating pairs of solar AlMg observations as function of separation time. The marked solid line indicates the median, while the other lines correspond to the 10, 25, 75, and 90% percentiles.
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$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f5.ps} \end{figure}$	Figure 5: The dots indicate the amplitude of X-ray variations observed in solar-type stars of Marino et al. (2002) in the band 0.7-2.4 keV vs. time scale. Arrows mark the median values of stars observed with time separation of the same order. The solid line marks the median value of the amplitude variations obtained from the AlMg Yohkoh observations of the Sun of Fig. 3.
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$\begin{figure} \par\includegraphics[angle=-90,width=12.8cm,clip]{b3460f6.ps} \end{figure}$	Figure 6: Residuals of the stellar amplitude variations from the solar median of Fig. 3 for stars in our sample versus time scale. Empty points mark stars with $\overline {L}_x <10^{28}$ erg/s while filled points are stars with $\overline {L}_x >10^{28}$ erg/s.
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