All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F1.ps} \end{figure}$ Figure 1: A typical blue part of the spectrum of CN Leo around 3200 Å. The emission lines belong to Fe I, Fe II, He I and He II.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F2.ps} \end{figure}$ Figure 2: Same as is Fig. 1 around 3600 Å. The emission lines belong to Ni I, Fe I, Cr I and He I.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F3.ps} \end{figure}$ Figure 3: Comparison of two models with dust (black) and without dust (red). The continuum is normalized for both models, otherwise the difference in the H $_{\alpha }$ line would cease.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F4.ps} \end{figure}$ Figure 4: Temperature structure for our best fit models. The solid line corresponds to AD Leo, the dotted line to YZ CMi, the dashed line to CN Leo, the dot-dashed line to LHS 3003 and the triple-dot-dashed line to DX Cnc. The models for AD Leo and YZ CMi are nearly identical.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F5.ps} \end{figure}$ Figure 5: Temperature structure for our best fit models of AD Leo. Given are the approximate line formation depths for various lines used in the fitting process.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F6.ps} \end{figure}$ Figure 6: Comparison of the observed spectrum of AD Leo (black) and the best fit model (grey/red). The emission cores/lines used for the modelling are indicated in the spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F7.ps} \end{figure}$ Figure 7: Same as is in Fig. 6. The absorption part of the Fe I line at 3720 Å, is too pronounced in the model what may be due to metalicity.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F8.ps} \end{figure}$ Figure 8: Comparison of the observed spectrum of YZ CMi (black) and the best fit model (grey/red). The H₉ is reproduced quite well. The Mg I lines show all less pronounced emission features in the model compared to the data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F9.ps} \end{figure}$ Figure 9: Same as is in Fig. 8 but for the Na I D lines. While the model shows deep self-absorption this is not seen in the data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F10.ps} \end{figure}$ Figure 10: Comparison between data (black) and model (grey/red) for CN Leo. Most of the Fe lines are too strong in the model.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F11.ps} \end{figure}$ Figure 11: Same as is in Fig. 10. Again the Fe lines are too strong while the three Balmer lines H₁₄ to H₁₆ are fitted quite well.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F12.ps} \end{figure}$ Figure 12: Comparison of data of DX Cnc (black) and best fit model (grey/red) for the H $_{\alpha }$ line. The model shows too deep self-absorption.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F13.ps} \end{figure}$ Figure 13: Comparison of data of LHS 3003 (black) and the best fit model (grey/red) for the H $_{\alpha }$ line. Here the self-absorption in the model is not deep enough.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F14.ps} \end{figure}$ Figure 14: Same as is in Fig. 13 but for the Na I D lines and the He I line at 5875 Å. The narrow emission lines are known airglow lines that have not been removed (see also Fig. A.1).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{A2338F15.ps} \end{figure}$ Figure 15: Comparison of two computations with different NLTE sets. The line at 3835.4 Å is H₉, the other lines are Fe I and Mg I. The Fe I and Mg I lines in the grey/red model often show much stronger line flux than in the black model since they are not computed in NLTE in the grey/red model. The H₉ line is influenced by the different NLTE sets of the two models, though hydrogen is computed in NLTE for both models. Further computations show that this is caused mainly by the different treatment of CNO in the two models.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F16.ps} \end{figure}$ Figure 16: Same comparison as in Fig. 15 for the Na I D line. The NLTE set that also includes Fe, Mg and CNO show shallower Na emission (black line) than the one that treats only H, He and Na in NLTE (grey/red line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F17.ps} \end{figure}$ Figure 17: Comparison of the influence of different NLTE sets on the electron density. The black line is the basic model with H, He and Na in NLTE. Grey/red is the model with Fe/Ni in NLTE and light grey/turquoise is the model with CNO I to CNO III in NLTE. All three models differ significantly in large parts of the atmosphere.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,height=5cm,clip=0]{A2338F18.ps} \end{figure}$ Figure A.1: Spectrum of 2MASSI J1315309-264951 around the Na I D lines. Known airglow lines for the UVES instrument are marked with a vertical line.

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F1.ps} \end{figure}$	Figure 1: A typical blue part of the spectrum of CN Leo around 3200 Å. The emission lines belong to Fe I, Fe II, He I and He II.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F2.ps} \end{figure}$	Figure 2: Same as is Fig. 1 around 3600 Å. The emission lines belong to Ni I, Fe I, Cr I and He I.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F3.ps} \end{figure}$	Figure 3: Comparison of two models with dust (black) and without dust (red). The continuum is normalized for both models, otherwise the difference in the H $_{\alpha }$ line would cease.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F4.ps} \end{figure}$	Figure 4: Temperature structure for our best fit models. The solid line corresponds to AD Leo, the dotted line to YZ CMi, the dashed line to CN Leo, the dot-dashed line to LHS 3003 and the triple-dot-dashed line to DX Cnc. The models for AD Leo and YZ CMi are nearly identical.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F5.ps} \end{figure}$	Figure 5: Temperature structure for our best fit models of AD Leo. Given are the approximate line formation depths for various lines used in the fitting process.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F6.ps} \end{figure}$	Figure 6: Comparison of the observed spectrum of AD Leo (black) and the best fit model (grey/red). The emission cores/lines used for the modelling are indicated in the spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F7.ps} \end{figure}$	Figure 7: Same as is in Fig. 6. The absorption part of the Fe I line at 3720 Å, is too pronounced in the model what may be due to metalicity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F8.ps} \end{figure}$	Figure 8: Comparison of the observed spectrum of YZ CMi (black) and the best fit model (grey/red). The H₉ is reproduced quite well. The Mg I lines show all less pronounced emission features in the model compared to the data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F9.ps} \end{figure}$	Figure 9: Same as is in Fig. 8 but for the Na I D lines. While the model shows deep self-absorption this is not seen in the data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F10.ps} \end{figure}$	Figure 10: Comparison between data (black) and model (grey/red) for CN Leo. Most of the Fe lines are too strong in the model.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F11.ps} \end{figure}$	Figure 11: Same as is in Fig. 10. Again the Fe lines are too strong while the three Balmer lines H₁₄ to H₁₆ are fitted quite well.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F12.ps} \end{figure}$	Figure 12: Comparison of data of DX Cnc (black) and best fit model (grey/red) for the H $_{\alpha }$ line. The model shows too deep self-absorption.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{A2338F13.ps} \end{figure}$	Figure 13: Comparison of data of LHS 3003 (black) and the best fit model (grey/red) for the H $_{\alpha }$ line. Here the self-absorption in the model is not deep enough.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{A2338F14.ps} \end{figure}$	Figure 14: Same as is in Fig. 13 but for the Na I D lines and the He I line at 5875 Å. The narrow emission lines are known airglow lines that have not been removed (see also Fig. A.1).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F16.ps} \end{figure}$	Figure 16: Same comparison as in Fig. 15 for the Na I D line. The NLTE set that also includes Fe, Mg and CNO show shallower Na emission (black line) than the one that treats only H, He and Na in NLTE (grey/red line).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{A2338F17.ps} \end{figure}$	Figure 17: Comparison of the influence of different NLTE sets on the electron density. The black line is the basic model with H, He and Na in NLTE. Grey/red is the model with Fe/Ni in NLTE and light grey/turquoise is the model with CNO I to CNO III in NLTE. All three models differ significantly in large parts of the atmosphere.
Open with DEXTER