All Figures

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6229F1.ps}\end{figure}$ Figure 1: X-ray light curve and hardness ratio of CN Leo from May 19/20, 2004 taken with the PN instrument with a bin size of 100 s. The vertical lines show the time interval of the simultaneous UVES observation.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{6229F2.ps}\hspace*{3.5mm} \includegraphics[width=8.05cm,clip]{6229F3.ps}\end{figure}$ Figure 2: Light curves in the optical and in X-rays plus an X-ray hardness ratio for 11 ( left) and 13 ( right) December 2005. The black curves denotes the XMM EPIC PN detector and the grey / light blue curves the blue UVES exposuremeter, which is scaled down in intensity by a factor of 30. The vertical dashed lines mark the beginning of the UVES exposures of the blue arm. Note that the steep rise of the exposuremeter data at the end of each UVES run is partly due to scattered light of the beginning dawn. The time bin size of the X-ray data is 100 s.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.7cm,clip]{6229F4.ps}\end{figure}$ Figure 3: PN spectra from the December 11th 2005 run (top/black), the December 13th run (middle/red), and the May 19th 2004 run (bottom/blue).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6229F5.ps}\end{figure}$ Figure 4: RGS spectrum of CN Leo constructed from RGS 1 and 2 in 1st order with the SAS task rgsfluxer from all three observations. Prominent emission features are labelled.
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In the text

$\begin{figure} \par\includegraphics[height=4.2cm,width=6.75cm,clip]{6229F6.ps}\end{figure}$ Figure 5: The (broad) forbidden coronal Fe XIII line at 3388 Å blended with the narrow chromospheric Ti II line; this spectrum is averaged from spectra 1 to 6 to increase the signal-to-noise ratio.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6229F7.ps}\end{figure}$ Figure 6: Spectral range around the H₉ line; various metal lines of Fe I and Mg I are indicated. The black spectrum is number 12 taken during the flare, the red/grey spectrum is number 1 from the December 11th 2005 run.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{6229F8.ps}\end{figure}$ Figure 7: Differential emission measure for CN Leo as determined by a 3rd-order polynomial fit (method 1) and a 4th-order polynomial fit (method 2) of line ratios from the combined RGS observations. Note that the shape of the $\it DEM$ at temperatures $\log T < 6$ cannot be determined from the available line ratios.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.35cm,clip]{6229F9.ps}\end{figure}$ Figure 8: Comparison of a synthetic spectrum based on the $\it DEM$ model and abundances from method 2 to the MOS1 (black) and MOS2 (red) spectra. The agreement is remarkably good, considering that the model has been determined independently from the EPIC data.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6229F10.ps}\end{figure}$ Figure 9: Variations in the line flux of the Fe XIII line and the corresponding emission measures of the cool, intermediate, and hot temperature component of the X-ray spectra. The vertical dashed line divides the two nights of the December 2005 observations. Note that flux variations within individual nights are not statistically significant.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{6229F11.ps}\end{figure}$ Figure 10: Line fluxes of various chromospheric emission lines. The black asterisks denote the He I D₃ line, the red diamonds the H $\beta$ line scaled down by a factor of 10, the blue crosses the Na I D line at 5889 Å, the green squares the H₉ line, and the yellow triangles the Ti II line at 3372 Å scaled up by a factor of 30. The vertical dashed line marks the onset of the second night.
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In the text

$\begin{figure} \par\includegraphics[width=6.95cm,clip]{6229F12.ps}\end{figure}$ Figure 11: Fit of the He II line in spectrum number 12. The histogram-like curve is the data from spectrum 12, the lower black curve the background as taken from spectrum 1. The upper black curve is the fit to the data and the dotted lines are the two Gaussians (with respect to the background).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6229F1.ps}\end{figure}$	Figure 1: X-ray light curve and hardness ratio of CN Leo from May 19/20, 2004 taken with the PN instrument with a bin size of 100 s. The vertical lines show the time interval of the simultaneous UVES observation.
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$\begin{figure} \par\includegraphics[angle=-90,width=6.7cm,clip]{6229F4.ps}\end{figure}$	Figure 3: PN spectra from the December 11th 2005 run (top/black), the December 13th run (middle/red), and the May 19th 2004 run (bottom/blue).
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6229F5.ps}\end{figure}$	Figure 4: RGS spectrum of CN Leo constructed from RGS 1 and 2 in 1st order with the SAS task `rgsfluxer` from all three observations. Prominent emission features are labelled.
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$\begin{figure} \par\includegraphics[height=4.2cm,width=6.75cm,clip]{6229F6.ps}\end{figure}$	Figure 5: The (broad) forbidden coronal Fe XIII line at 3388 Å blended with the narrow chromospheric Ti II line; this spectrum is averaged from spectra 1 to 6 to increase the signal-to-noise ratio.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{6229F7.ps}\end{figure}$	Figure 6: Spectral range around the H₉ line; various metal lines of Fe I and Mg I are indicated. The black spectrum is number 12 taken during the flare, the red/grey spectrum is number 1 from the December 11th 2005 run.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{6229F8.ps}\end{figure}$	Figure 7: Differential emission measure for CN Leo as determined by a 3rd-order polynomial fit (method 1) and a 4th-order polynomial fit (method 2) of line ratios from the combined RGS observations. Note that the shape of the $\it DEM$ at temperatures $\log T < 6$ cannot be determined from the available line ratios.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.35cm,clip]{6229F9.ps}\end{figure}$	Figure 8: Comparison of a synthetic spectrum based on the $\it DEM$ model and abundances from method 2 to the MOS1 (black) and MOS2 (red) spectra. The agreement is remarkably good, considering that the model has been determined independently from the EPIC data.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{6229F10.ps}\end{figure}$	Figure 9: Variations in the line flux of the Fe XIII line and the corresponding emission measures of the cool, intermediate, and hot temperature component of the X-ray spectra. The vertical dashed line divides the two nights of the December 2005 observations. Note that flux variations within individual nights are not statistically significant.
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$\begin{figure} \par\includegraphics[width=6.95cm,clip]{6229F12.ps}\end{figure}$	Figure 11: Fit of the He II line in spectrum number 12. The histogram-like curve is the data from spectrum 12, the lower black curve the background as taken from spectrum 1. The upper black curve is the fit to the data and the dotted lines are the two Gaussians (with respect to the background).
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