Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=8.6cm,height=5cm,clip]{1941f1a.eps}\vs... ...ce*{2mm} \par\includegraphics[width=8.6cm,height=5cm,clip]{1941f1d} \end{figure}$ Figure 1: Light curves of the binaries EQ Peg and AT Mic and the single stars AD Leo and EV Lac; PN (+MOS2/red) data, 100 s binning. Frequent flaring is observed on various timescales; selected flaring periods are indicated by horizontal arrows.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1941f3} \end{figure}$ Figure 3: PN spectra of the analysed M dwarfs; top to bottom: AT Mic (red), AD Leo (green), EV Lac (blue), EQ Peg (black). ( Colour figure in electronic version.)
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1941f4} \end{figure}$ Figure 4: EMDs as derived with the 6-T model and scaled with the summed abundance of iron and oxygen, total observation each (RGS: Asterisks, MOS: Diamonds, PN: Squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1941f5} \end{figure}$ Figure 5: Elemental abundances in stellar coronae relative to solar photospheric values vs. FIP for our sample stars; an inverse FIP effect is present in all stars. Each star is shifted by one solar abundance on the vertical axis, the dashed lines indicate 0.5 solar abundance in each case.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.55cm,clip]{1941f6} \end{figure}$ Figure 6: Spectra of AT Mic during different states of activity, PN data from selected time-intervals as defined in Table 3 (high: black, medium: green, qq: red). ( Colour figure in electronic version.)
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,height=5.1cm,clip]{1941f7a}\par\vspace*{4mm} \includegraphics[width=8.4cm,height=5.1cm,clip]{1941f7b} \end{figure}$ Figure 7: EMDs of our sample M dwarfs in different states of activity derived from PN data. The upper plot shows the flaring phase, for AT Mic the medium activity phase is additionally plotted as a dashed line while the lower plot shows the quasi-quiescent state. Undetected components are plotted with their upper limits, denoted by downward arrows.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,height=5cm,clip]{1941f1a.eps}\vs... ...ce*{2mm} \par\includegraphics[width=8.6cm,height=5cm,clip]{1941f1d} \end{figure}$	Figure 1: Light curves of the binaries EQ Peg and AT Mic and the single stars AD Leo and EV Lac; PN (+MOS2/red) data, 100 s binning. Frequent flaring is observed on various timescales; selected flaring periods are indicated by horizontal arrows.
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$\begin{figure} \par\includegraphics[width=8.4cm,height=7.6cm,clip]{1941f2} \end{figure}$	Figure 2: RGS spectra of the sample stars, the most prominent emission features are labelled.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{1941f3} \end{figure}$	Figure 3: PN spectra of the analysed M dwarfs; top to bottom: AT Mic (red), AD Leo (green), EV Lac (blue), EQ Peg (black). ( Colour figure in electronic version.)
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1941f4} \end{figure}$	Figure 4: EMDs as derived with the 6-T model and scaled with the summed abundance of iron and oxygen, total observation each (RGS: Asterisks, MOS: Diamonds, PN: Squares).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1941f5} \end{figure}$	Figure 5: Elemental abundances in stellar coronae relative to solar photospheric values vs. FIP for our sample stars; an inverse FIP effect is present in all stars. Each star is shifted by one solar abundance on the vertical axis, the dashed lines indicate 0.5 solar abundance in each case.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.55cm,clip]{1941f6} \end{figure}$	Figure 6: Spectra of AT Mic during different states of activity, PN data from selected time-intervals as defined in Table 3 (high: black, medium: green, qq: red). ( Colour figure in electronic version.)
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$\begin{figure} \par\includegraphics[width=8.4cm,height=5.1cm,clip]{1941f7a}\par\vspace*{4mm} \includegraphics[width=8.4cm,height=5.1cm,clip]{1941f7b} \end{figure}$	Figure 7: EMDs of our sample M dwarfs in different states of activity derived from PN data. The upper plot shows the flaring phase, for AT Mic the medium activity phase is additionally plotted as a dashed line while the lower plot shows the quasi-quiescent state. Undetected components are plotted with their upper limits, denoted by downward arrows.
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