All Figures

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F1.ps} \end{figure}$ Figure 1: Temperature vs. column mass distribution for the flare models on a logarithmic scale. The black line denotes the best fit model out of the grid.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F2.ps} \end{figure}$ Figure 2: Light curve of LHS 2034 during the observation on March 14th, 2002. The upper light curve corresponds to the red part of the spectrum, while the lower light curve corresponds to the blue part. The flare can be seen clearly in both spectral ranges. The vertical dashed lines indicate the beginning of each exposure. The flare ends at about the beginning of the third exposure.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F3.ps} \end{figure}$ Figure 3: Spectral sequence of the H $_{\beta }$ line on a logarithmic plot. Note the large asymmetries in the second and third spectra: in the red wing there is considerably more flux than in the blue.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F4.ps}\par \end{figure}$ Figure 4: Spectral wavelength around the He I D₃ line at 5875 Å and the Na D lines at 5890 and 5896 Å in the second spectrum of the series. Though the strength of the line is about the same, the He I D₃ line shows red wing asymmetry while the Na D lines does not. All other (narrow) emission lines seen in this part of the spectrum are known airglow lines.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F5.ps} \end{figure}$ Figure 5: Example of the three-component fit of the He I D₃ line in the second spectrum. Plotted are all three components, the resulting fit, and the data.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F6.ps} \end{figure}$ Figure 6: Fit of the H $_{\alpha }$ line with two components. The amplitude of the narrow component was fitted manually due to the severe self-absorption. The fit parameters can be found in Table 3 for Spectrum 2.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F7.ps} \end{figure}$ Figure 7: Ratio of the amplitude of the broad line component to the narrow line component. The ratio between the main component of the He I D₃ line and its broad component is named "He b'', and between the main component and the second component it is named "He 2''.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F8.ps} \end{figure}$ Figure 8: Line shift between the narrow and the broad component of the different lines. Error should be typically about 10 ${\rm km~s^{-1}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F9.ps} \end{figure}$ Figure 9: Comparison of model (grey/red) and the first flare spectrum of LHS 2034 (black) around H $_{\alpha }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F10.ps} \end{figure}$ Figure 10: Comparison of model (grey/red) and the first flare spectrum of LHS 2034 (black) around the Na D lines and the He I D₃ line. While the He line is slightly overpredicted, the Na D lines are vastly underpredicted. The narrow airglow lines are found in the model since we used a quiescent observed spectrum to mix with.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F11.ps} \end{figure}$ Figure 11: Comparison of the He I D₃ line for a number of program stars. The black line denotes LHS 2034 where the asymmetry can be seen clearly. Also plotted are the flare spectrum of LHS 2076 (grey/red), the strongest CN Leo spectrum (light grey/turquoise), and the averaged spectrum of GL Vir (dotted) and of YZ Cmi (dashed). No strong wing asymmetries are found in the other spectra, except the bump that originates from the reddest line component.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F12.ps} \end{figure}$ Figure 12: The H $_{\alpha }$ line for LHS 2397a. While the first two spectra show enhanced H $_{\alpha }$ flux and some red wing asymmetries, the third spectrum fits well with only one component.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F1.ps} \end{figure}$	Figure 1: Temperature vs. column mass distribution for the flare models on a logarithmic scale. The black line denotes the best fit model out of the grid.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F2.ps} \end{figure}$	Figure 2: Light curve of LHS 2034 during the observation on March 14th, 2002. The upper light curve corresponds to the red part of the spectrum, while the lower light curve corresponds to the blue part. The flare can be seen clearly in both spectral ranges. The vertical dashed lines indicate the beginning of each exposure. The flare ends at about the beginning of the third exposure.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F3.ps} \end{figure}$	Figure 3: Spectral sequence of the H $_{\beta }$ line on a logarithmic plot. Note the large asymmetries in the second and third spectra: in the red wing there is considerably more flux than in the blue.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F4.ps}\par \end{figure}$	Figure 4: Spectral wavelength around the He I D₃ line at 5875 Å and the Na D lines at 5890 and 5896 Å in the second spectrum of the series. Though the strength of the line is about the same, the He I D₃ line shows red wing asymmetry while the Na D lines does not. All other (narrow) emission lines seen in this part of the spectrum are known airglow lines.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F5.ps} \end{figure}$	Figure 5: Example of the three-component fit of the He I D₃ line in the second spectrum. Plotted are all three components, the resulting fit, and the data.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F6.ps} \end{figure}$	Figure 6: Fit of the H $_{\alpha }$ line with two components. The amplitude of the narrow component was fitted manually due to the severe self-absorption. The fit parameters can be found in Table 3 for Spectrum 2.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F7.ps} \end{figure}$	Figure 7: Ratio of the amplitude of the broad line component to the narrow line component. The ratio between the main component of the He I D₃ line and its broad component is named "He b'', and between the main component and the second component it is named "He 2''.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F8.ps} \end{figure}$	Figure 8: Line shift between the narrow and the broad component of the different lines. Error should be typically about 10 ${\rm km~s^{-1}}$ .
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F9.ps} \end{figure}$	Figure 9: Comparison of model (grey/red) and the first flare spectrum of LHS 2034 (black) around H $_{\alpha }$ .
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F10.ps} \end{figure}$	Figure 10: Comparison of model (grey/red) and the first flare spectrum of LHS 2034 (black) around the Na D lines and the He I D₃ line. While the He line is slightly overpredicted, the Na D lines are vastly underpredicted. The narrow airglow lines are found in the model since we used a quiescent observed spectrum to mix with.
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$\begin{figure} \par\includegraphics[width=8cm,height=5cm,clip=0]{A2518F12.ps} \end{figure}$	Figure 12: The H $_{\alpha }$ line for LHS 2397a. While the first two spectra show enhanced H $_{\alpha }$ flux and some red wing asymmetries, the third spectrum fits well with only one component.
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