$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0054fig1.ps}} \end{figure}$ Figure 1: Background-subtracted and pileup-corrected lightcurves for EQ Peg A ( top) and B ( bottom). Binsize for both sources is 600 s.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig2.ps}} \end{figure}$ Figure 2: Chandra MEG spectra of EQ Peg A ( top, red) and B ( bottom, blue). Both spectra have been rebinned.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig3.eps}} \end{figure}$ Figure 3: Cumulative distribution ( top) of counts in the MEG spectra of EQ Peg A (dotted line: all data, solid line: with the two larger flares on 28th November and December $1{\rm st}$ excluded) and B (dashed line); and ratio B/A ( middle panel: all data, bottom: with the two larger flares on EQ Peg A excluded).
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig4.ps}} \end{figure}$ Figure 4: Spectral region around the Ne X line at 12.13 Å and the Fe XVII and Fe XXI lines at 12.26 and 12.28 Å in the total spectrum of EQ Peg A.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig5.ps}} \end{figure}$ Figure 5: The Ne IX triplet in the MEG spectra of EQ Peg A during the four observations. On observation No. 8485 the flare spectrum only is overlaid in gray.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig8.ps}} \end{figure}$ Figure 7: Line emissivity curves for different H-like and He-like ions, and Fe XVII at 15.01 Å from CHIANTI 5.2 (Landi et al. 2006) with the ionization balance from Mazzotta et al. (1998).
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig9.ps}} \end{figure}$ Figure 8: Best-fit linear combination of the contribution functions of the H-like Ly $\alpha$ and He-like resonance lines of silicon and magnesium.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fi10.eps}} \end{figure}$ Figure 9: Cumulative distribution of counts in the quiescent spectra of the reference star Capella and other M dwarfs observed with the Chandra HETGS. The area between the curves for EQ Peg A and B is indicated in shades of gray for comparison.
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In the text

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fi11.ps}} \end{figure}$ Figure 10: Relative abundances as a function of spectral type derived from the seven M dwarfs as listed in Tables 7 and 10.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{0054fig1.ps}} \end{figure}$	Figure 1: Background-subtracted and pileup-corrected lightcurves for EQ Peg A ( top) and B ( bottom). Binsize for both sources is 600 s.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig2.ps}} \end{figure}$	Figure 2: Chandra MEG spectra of EQ Peg A ( top, red) and B ( bottom, blue). Both spectra have been rebinned.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig3.eps}} \end{figure}$	Figure 3: Cumulative distribution ( top) of counts in the MEG spectra of EQ Peg A (dotted line: all data, solid line: with the two larger flares on 28th November and December $1{\rm st}$ excluded) and B (dashed line); and ratio B/A ( middle panel: all data, bottom: with the two larger flares on EQ Peg A excluded).
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig4.ps}} \end{figure}$	Figure 4: Spectral region around the Ne X line at 12.13 Å and the Fe XVII and Fe XXI lines at 12.26 and 12.28 Å in the total spectrum of EQ Peg A.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig5.ps}} \end{figure}$	Figure 5: The Ne IX triplet in the MEG spectra of EQ Peg A during the four observations. On observation No. 8485 the flare spectrum only is overlaid in gray.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig6.ps}}\\ \resizebox{9cm}{!}{\includegraphics{0054fig7.ps}} \end{figure}$	Figure 6: Differential emission measures of EQ Peg A ( top) and B ( bottom) for the total observation time (i.e. flare and quiescence).
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$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig8.ps}} \end{figure}$	Figure 7: Line emissivity curves for different H-like and He-like ions, and Fe XVII at 15.01 Å from CHIANTI 5.2 (Landi et al. 2006) with the ionization balance from Mazzotta et al. (1998).
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fig9.ps}} \end{figure}$	Figure 8: Best-fit linear combination of the contribution functions of the H-like Ly $\alpha$ and He-like resonance lines of silicon and magnesium.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fi10.eps}} \end{figure}$	Figure 9: Cumulative distribution of counts in the quiescent spectra of the reference star Capella and other M dwarfs observed with the Chandra HETGS. The area between the curves for EQ Peg A and B is indicated in shades of gray for comparison.
Open with DEXTER

$\begin{figure} \par\resizebox{9cm}{!}{\includegraphics{0054fi11.ps}} \end{figure}$	Figure 10: Relative abundances as a function of spectral type derived from the seven M dwarfs as listed in Tables 7 and 10.
Open with DEXTER