$\begin{figure} \par\hspace*{2mm}\includegraphics[width=6.72cm,clip]{0494fig1.eps... ...ig2.eps}\vspace*{5mm} \includegraphics[width=7cm,clip]{0494fig3.eps}\end{figure}$ Figure 1: Light curves and hardness ratio of 44 Boo. In the top panel, the upper curve is the count rate in the 0.3 to 2 keV band and the lower curve is the count rate in the 2 to 10 keV band. This light curve is expanded in the middle panel. The lower panel shows the hardness ratio between the high and low energy bands. The events are binned in 180 s time intervals and the background contribution has been subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0494fig4.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{0494fig5.ps}\end{figure}$ Figure 2: Best fit MEKAL model (see Table 3) to EPIC spectra during the flare periods ( left) and during the intermediate steady flux period ( right). The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. Their ratio is shown in the lower panel of each graph.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0494fig6.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{0494fig7.ps}\end{figure}$ Figure 3: Best fit model (using a power-law emission measure distribution; see Table 4) to EPIC spectra during the flare periods ( left) and during the intermediate steady flux period ( right). The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. Their ratio is shown in the lower panel of each graph.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{0494fig9.eps}\end{figure}$ Figure 5: Comparison of RGS 2 data with a best fit model folded with RGS2 response matrix. The model consists a three temperature Bremstrahlung continuum and Gaussian lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0494fig10.ps}\hspace*{1.5cm} \includegraphics[width=7.55cm,clip]{0494fig11.ps}\end{figure}$ Figure 6: Left: intensity ratio R = f/i of the O VII forbiden ( $\lambda$ = 22.12 Å) and intercombination ( $\lambda$ = 21.80 Å) lines as a function of electron density. Right: ratio G = (i + f)/r of the summed intensities of the OVII intercombination and forbiden lines over the intensity of the recombination line ( $\lambda$ = 21.60 Å) calculated using the CHIANTI database (Dere et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0494fig12.eps}\end{figure}$ Figure 7: Comparison between the emission measure distributions derived from EPIC flares and quiescent periods (see Table 3) and from Fe, Ne and O line fluxes in RGS spectrum (see Table 5).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0494fig4.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{0494fig5.ps}\end{figure}$	Figure 2: Best fit MEKAL model (see Table 3) to EPIC spectra during the flare periods ( left) and during the intermediate steady flux period ( right). The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. Their ratio is shown in the lower panel of each graph.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0494fig6.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{0494fig7.ps}\end{figure}$	Figure 3: Best fit model (using a power-law emission measure distribution; see Table 4) to EPIC spectra during the flare periods ( left) and during the intermediate steady flux period ( right). The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. Their ratio is shown in the lower panel of each graph.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{0494fig8.eps}\end{figure}$	Figure 4: RGS spectrum of 44 Boo in the 6-38 Å band.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{0494fig9.eps}\end{figure}$	Figure 5: Comparison of RGS 2 data with a best fit model folded with RGS2 response matrix. The model consists a three temperature Bremstrahlung continuum and Gaussian lines.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0494fig12.eps}\end{figure}$	Figure 7: Comparison between the emission measure distributions derived from EPIC flares and quiescent periods (see Table 3) and from Fe, Ne and O line fluxes in RGS spectrum (see Table 5).
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