All Figures

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8848fig1.eps}\end{figure}$ Figure 1: Light curves of the flares extracted from EPIC-pn, except for $\xi$ Boo flare that was extracted from EPIC-MOS. Time segments used for flare and quiescence spectra extraction are marked by F and Q respectively. CC Eri and $\sigma$ Gem show no clear quiescence during the observation and therefore a different observation was used as quiescence reference. See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{8848fig2.eps}\end{figure}$ Figure 2: FeEMD solutions for the flare (orange) and quiescence (blue). Errors are 1 $\sigma$ and include uncertainties due to correlation between the bins. Dashed lines represent the polynomial parameterized solutions.
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In the text

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8848fig3.eps}\end{figure}$ Figure 3: FeIEM results for flare (orange) and quiescent (blue) states, namely the progressive integral over the FeEMD of Fig. 2. Plotted errors account for uncertainties due to correlations between bins during integration. Dotted lines show the results of the integration over the polynomial parameterized FeEMD (see Fig. 2).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{8848fig4.eps}\end{figure}$ Figure 4: Flare abundances relative to quiescence, as a function of FIP. Elements observed with the RGS (O, Ne, Mg, Si) are considered the most reliable and are marked in red. Those observed only with the low-resolution EPIC instruments are marked black. Elements whose abundance determination depends on the EMD below temperatures of kT=0.1 keV, for which we did not solve, may suffer from systematic errors and are plotted in gray. The vertical dotted line mark the FIP of of the reference element Fe.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8848fig5.eps}\end{figure}$ Figure 5: The FIP bias measure FB, defined in Eq. (5), of the flare plasma relative to quiescence as a function of the FB of the corona in quiescence, relative to Solar (photospheric). Black circles are from XMM-Newton observations, blue squares are from Chandra (Paper I) violet diamonds are for solar flares.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8848fig6.eps}\end{figure}$ Figure 6: Absolute value of FIP bias measure FB as a function of the ratio of integrated EM from 0.1 to 1 keV in the flare relative to quiescence. A low-T EM excess is required in order to enable the detection of abundance variations of the key elements O, Ne, Mg and Si.
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In the text

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8848fig1.eps}\end{figure}$	Figure 1: Light curves of the flares extracted from EPIC-pn, except for $\xi$ Boo flare that was extracted from EPIC-MOS. Time segments used for flare and quiescence spectra extraction are marked by F and Q respectively. CC Eri and $\sigma$ Gem show no clear quiescence during the observation and therefore a different observation was used as quiescence reference. See text for details.
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{8848fig2.eps}\end{figure}$	Figure 2: FeEMD solutions for the flare (orange) and quiescence (blue). Errors are 1 $\sigma$ and include uncertainties due to correlation between the bins. Dashed lines represent the polynomial parameterized solutions.
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$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8848fig3.eps}\end{figure}$	Figure 3: FeIEM results for flare (orange) and quiescent (blue) states, namely the progressive integral over the FeEMD of Fig. 2. Plotted errors account for uncertainties due to correlations between bins during integration. Dotted lines show the results of the integration over the polynomial parameterized FeEMD (see Fig. 2).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8848fig5.eps}\end{figure}$	Figure 5: The FIP bias measure FB, defined in Eq. (5), of the flare plasma relative to quiescence as a function of the FB of the corona in quiescence, relative to Solar (photospheric). Black circles are from XMM-Newton observations, blue squares are from Chandra (Paper I) violet diamonds are for solar flares.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8848fig6.eps}\end{figure}$	Figure 6: Absolute value of FIP bias measure FB as a function of the ratio of integrated EM from 0.1 to 1 keV in the flare relative to quiescence. A low-T EM excess is required in order to enable the detection of abundance variations of the key elements O, Ne, Mg and Si.
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