$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0911fig1.eps} \end{figure}$ Figure 1: EIT 195 Å images of the observed active region at two times, showing the position of the SUMER slit, indicated by the vertical line.
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In the text

$\begin{figure} \par\includegraphics[width=8.0cm,height=4.8cm,angle=0]{0911fig2.eps} \end{figure}$ Figure 2: Time series of line radiance along the SUMER spectrometer slit for the period 16 Sep. 19:00 UT to 17 Sep. 7:36 UT. The distance in pixels along the SUMER slit is shown on the vertical axis.
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In the text

$\begin{figure} \par\includegraphics[width=7.5 cm]{0911fig3.eps} \end{figure}$ Figure 3: Distribution functions of SUMER data in the active region corona (solid lines) and best fit lognormal functions (dashed lines). The radiances are normalized to their median and their distributions to the number of data points.
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In the text

$\begin{figure} \par\includegraphics[width=8.1 cm,clip]{0911fig4.eps} \end{figure}$ Figure 4: Light curves for flare models run with different $\tau$ , p_f and $\alpha$ parameters. All light curves have $\tau p_f = 2$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0911fig6.eps} \end{figure}$ Figure 6: Samples of the radiance time series: left panel: SUMER data, and right panel: simulation data obtained with the parameters given in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0911fig1.eps} \end{figure}$	Figure 1: EIT 195 Å images of the observed active region at two times, showing the position of the SUMER slit, indicated by the vertical line.
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$\begin{figure} \par\includegraphics[width=8.0cm,height=4.8cm,angle=0]{0911fig2.eps} \end{figure}$	Figure 2: Time series of line radiance along the SUMER spectrometer slit for the period 16 Sep. 19:00 UT to 17 Sep. 7:36 UT. The distance in pixels along the SUMER slit is shown on the vertical axis.
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$\begin{figure} \par\includegraphics[width=7.5 cm]{0911fig3.eps} \end{figure}$	Figure 3: Distribution functions of SUMER data in the active region corona (solid lines) and best fit lognormal functions (dashed lines). The radiances are normalized to their median and their distributions to the number of data points.
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$\begin{figure} \par\includegraphics[width=8.1 cm,clip]{0911fig4.eps} \end{figure}$	Figure 4: Light curves for flare models run with different $\tau$ , p_f and $\alpha$ parameters. All light curves have $\tau p_f = 2$ .
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$\begin{figure} \par\includegraphics[width=7.5 cm,angle=0,clip]{0911fig5.eps} \end{figure}$	Figure 5: Schematic of a typical probabilistic neural network.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0911fig6.eps} \end{figure}$	Figure 6: Samples of the radiance time series: left panel: SUMER data, and right panel: simulation data obtained with the parameters given in Table 1.
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