All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5065f1_c.eps}\end{figure}$ Figure 1: TRACE image (logarithmic scale) in the 17.1 nm band showing AR 10061 at flare peak. The dark grey (red in the electronic version) box indicates the UBF FOV while the area rastered by CDS/NIS is represented by the light grey (blue) box. The white vertical line marks the position of the DST spectrograph slit. Here and in the following images, the white dashed line shows the apparent magnetic inversion line obtained from MDI data in the region around the filament.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5065f2.eps} \end{figure}$ Figure 2: Soft X-ray full disk flux at 1 UA in the 1 to 8 Å band around the time of the flare (GOES 8 data). The time derivative (dashed line) represents a proxy for the hard X-ray curve (Neupert effect) and shows its maximum around 14:41:20 UTC.
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In the text

$\begin{figure} \includegraphics[width=11.6cm,clip]{5065f3_c.eps} \end{figure}$ Figure 3: Evolution of the flare: TRACE images (logarithmic scale) in the 17.1 nm band are shown in the first two rows and H $\alpha$ images in the last two rows. The white box in TRACE images indicate the H $\alpha$ FOV. The images at 14:34 UTC show the region just before the flare. The areas (labelled A and B) over which data were integrated to obtain the light and velocity curves shown in Fig. 4 are indicated in black on the TRACE image taken at 14:42:00 UTC. The arrow in the last H $\alpha$ image indicates the cool post-flare loops.
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In the text

$\begin{figure} \par\includegraphics[width=10.7cm,clip]{5065f4.eps} \end{figure}$ Figure 4: Light and velocity curves at the footpoints (areas A and B in Fig. 3) of the loop system. For clarity reasons uncertainties are only shown for the Fe XIX speeds. O V, Fe XVI, and TRACE radiances are normalised to pre-flare values while Fe XIX radiances are normalised to the average value reached after the flare (around 15:32 UTC). The average uncertainties in the normalised radiance are of about 0.15. On footpoint A, the average uncertainties in speed are 12 km s^-1 (O V) and 20 km s^-1 (Fe XVI). On footpoint B, the average uncertainties in speed are 9 and 12 km s^-1 for O V and Fe XVI. The shaded area represents the time during which downflows between 4 and 10 km s^-1 were observed in H $\alpha$ . (We remind that only for footpoint B we have chromospheric observations). On both panels, the scale of downward (positive) velocities has been expanded for sake of clarity.
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In the text

$\begin{figure} \includegraphics[width=10.3cm,clip]{5065f5.eps} \end{figure}$ Figure 5: Eastward ribbon (A) at 14:40:45 UTC. The top left panel shows a TRACE image in the 17.1 nm band. The bottom left panel shows a map of the O V LOS velocity within the area encompassed by the black box on the TRACE image. On both panels isocontours of the O V radiances at a level of 5 W m² sr^-1 are shown with white thick lines while the thick black isocontours on the velocity map indicate Fe XIX radiances at a level of 90 mW m² sr^-1. The Fe XIX profile shown in the top-right panel is obtained by integrating over three pixels along the CDS slit, centred at the location indicated by a white x on the velocity map (area A defined in Fig. 3). The single pixel O V profiles on the bottom right panel refer to the locations indicated by a black + (thick histogram) and a white + (thin histogram) on the velocity map.
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In the text

$\begin{figure} \includegraphics[width=10.27cm,clip]{5065f6.eps} \end{figure}$ Figure 6: Eastward ribbon (A) at 14:44 UTC. The top left panel shows a TRACE image in the 17.1 nm band while the H $\alpha$ image closest in time is shown in the top right panel. On both images the thin black contours indicate chromospheric downflows of 4 km s^-1. The Fe XIX line profile shown on the bottom panel is obtained by integrating over three pixels along the CDS slit (area A defined in Fig. 3).
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In the text

$\begin{figure} \includegraphics[width=10.27cm,clip]{5065f7.eps} \end{figure}$ Figure 7: Westward ribbon (B) at 14:42 UTC. Panels are as in Fig. 6. On both images the thin black contours indicate chromospheric downflows of 4 km s^-1 and 7 km s^-1. The Fe XIX line profile shown on the bottom panel is obtained by integrating over the area within white solid lines in the H $\alpha$ image (area B defined in Fig. 3). A single component fit (plus background) would result in an upflow speed of ( $-125\pm 50$ ) km s^-1.
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In the text

$\begin{figure} \includegraphics[width=10.3cm,clip]{5065f8.eps} \end{figure}$ Figure 8: Gradual phase at a time when the CDS slit was crossing the western footpoint. The top left panel shows a TRACE image in the 17.1 nm band while the H $\alpha$ image closest in time is shown in the top right panel. On the TRACE image isocontours of the Fe XIX radiance at levels of (0.11, 0.22) W m^-2 sr^-1 are indicated by thick white solid lines. On the H $\alpha$ image, instead, the white thick contours refer to a RHESSI image obtained between 14:50 and 14:51 UTC in the 6 to 12 keV band. The contours are traced at levels of 40% and 75% of the maximum. The Fe XIX line profile shown on the bottom panel is obtained by integrating over the areas within white solid thin lines in the H $\alpha$ image (area B). In this case the radiance of the rest component (dashed line) was set to zero. The dotted line indicates the background (lines plus constant background) defined from pre-flare spectra. The thick solid line indicates the fitted profile.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.2cm,clip]{5065f9a.eps}\hspace*{10mm} \includegraphics[width=7.2cm,clip]{5065f9b.eps} } \end{figure}$ Figure 9: RHESSI spectra in the 4 to 10 keV energy range at 14:50 UTC ( left panel) and at 15:13 UTC ( right panel). Notice the presence of a broadened emission feature at about 6.6 keV corresponding to a group of emission lines due to Fe XXIV-XXVI.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{5065f10.eps} \end{figure}$ Figure 10: Cooling curve obtained from the time of maximum appearance of progressively colder features. RHESSI temperature at 14:50 UTC refers to the thermal component (see left panel of Fig. 9). Each set of curves (thin and thick) refer to three different values of the volumetric filling factor f (0.1, dot-dashed; 0.3, dashed; 0.5, dotted). The solid part of the curves indicates the times when conduction dominates, while the non-solid part indicates the time when the plasma cools radiatively. The thick curves are obtained assuming constant density only during the conductive phase, while the thin curves are obtained assuming constant density through the entire cooling (see text).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5065f2.eps} \end{figure}$	Figure 2: Soft X-ray full disk flux at 1 UA in the 1 to 8 Å band around the time of the flare (GOES 8 data). The time derivative (dashed line) represents a proxy for the hard X-ray curve (Neupert effect) and shows its maximum around 14:41:20 UTC.
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$\begin{figure} \par\mbox{\includegraphics[width=7.2cm,clip]{5065f9a.eps}\hspace*{10mm} \includegraphics[width=7.2cm,clip]{5065f9b.eps} } \end{figure}$	Figure 9: RHESSI spectra in the 4 to 10 keV energy range at 14:50 UTC ( left panel) and at 15:13 UTC ( right panel). Notice the presence of a broadened emission feature at about 6.6 keV corresponding to a group of emission lines due to Fe XXIV-XXVI.
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