All Figures

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{h4146F1.ps} \end{figure}$ Figure 1: H-R diagram of single giants (Gondoin 1999) compared with evolutionary tracks (Schaller et al. 1992) of 1 $M_\odot$ (lower dashed line), 1.25 $M_\odot$ , 1.5 $M_\odot$ , 1.7 $M_\odot$ (solid line), 2 $M_\odot$ and 2.5 $M_\odot$ . Black circles mark giants known as X-ray sources. The H-R diagram location of V390 Aurigae is indicated by an error bar.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{h4146F2.ps}\hspace*{4mm} \includegraphics[angle=270,width=7.2cm,clip]{h4146F3.ps} \end{figure}$ Figure 2: Light curves of V390 Aurigae during revolutions 135 (left) and 232 (right) obtained with the EPIC p-n camera. In each graph, the upper curve is the count rate within the 0.3 to 2 keV band and the lower curve is the count rate within the 2 to 10 keV band. The events are binned in 300 s time intervals and the background has been subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{h4146F4.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{h4146F5.ps} \end{figure}$ Figure 3: Best fit model to revolution 135 (left) and 232 (right) spectra. The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel of each graph.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{h4146F6.ps}\par\vspace*{3mm} \includegraphics[width=8.4cm,clip]{h4146F7.ps} \end{figure}$ Figure 4: Averaged first order spectra of RGS 1 and 2 obtained during revolution 135 (top) and revolution 232 (bottom).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{h4146F8.ps} \end{figure}$ Figure 5: Equatorial rotational velocity of V390 Aurigae (filled circle) compared with $v \sin i$ values of single field giants (Gondoin 1999). The solid line and the dashed line describe the equatorial velocity evolution of 1.7 $M_\odot$ and 2.5 $M_\odot$ stars respectively assuming angular momentum conservation and $v \sin i = 150$ km s^-1 at $T_{\rm eff}= 7000$ K.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{h4146F9.ps} \end{figure}$ Figure 6: The error bars in the upper part of the graph indicate the XMM-Newton luminosity range of FK Comae and of V390 Aurigae (bold bar) in the 0.3 to 2 keV band compared with ROSAT PSPC measurements of single field giants (Hünsch et al. 1998). Upper limits of X-ray luminosities measured with the Einstein observatory (Maggio et al. 1990) are indicated by small triangles, large triangles and filled triangles for low-mass (1.2 $M_\odot < M < 2.0~M_\odot$ ), intermediate-mass (2.0 $M_\odot < M < 2.5$ $M_\odot$ ) and clump giants respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{h4146F1.ps} \end{figure}$	Figure 1: H-R diagram of single giants (Gondoin 1999) compared with evolutionary tracks (Schaller et al. 1992) of 1 $M_\odot$ (lower dashed line), 1.25 $M_\odot$ , 1.5 $M_\odot$ , 1.7 $M_\odot$ (solid line), 2 $M_\odot$ and 2.5 $M_\odot$ . Black circles mark giants known as X-ray sources. The H-R diagram location of V390 Aurigae is indicated by an error bar.
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$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{h4146F2.ps}\hspace*{4mm} \includegraphics[angle=270,width=7.2cm,clip]{h4146F3.ps} \end{figure}$	Figure 2: Light curves of V390 Aurigae during revolutions 135 (left) and 232 (right) obtained with the EPIC p-n camera. In each graph, the upper curve is the count rate within the 0.3 to 2 keV band and the lower curve is the count rate within the 2 to 10 keV band. The events are binned in 300 s time intervals and the background has been subtracted.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{h4146F4.ps}\hspace*{4mm} \includegraphics[angle=270,width=8cm,clip]{h4146F5.ps} \end{figure}$	Figure 3: Best fit model to revolution 135 (left) and 232 (right) spectra. The EPIC data (crosses) and spectral fit (solid line) are shown in the upper panel. The $\chi ^{2}$ contributions are given in the lower panel of each graph.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{h4146F6.ps}\par\vspace*{3mm} \includegraphics[width=8.4cm,clip]{h4146F7.ps} \end{figure}$	Figure 4: Averaged first order spectra of RGS 1 and 2 obtained during revolution 135 (top) and revolution 232 (bottom).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{h4146F8.ps} \end{figure}$	Figure 5: Equatorial rotational velocity of V390 Aurigae (filled circle) compared with $v \sin i$ values of single field giants (Gondoin 1999). The solid line and the dashed line describe the equatorial velocity evolution of 1.7 $M_\odot$ and 2.5 $M_\odot$ stars respectively assuming angular momentum conservation and $v \sin i = 150$ km s^-1 at $T_{\rm eff}= 7000$ K.
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