$\begin{figure} \par\mbox{\includegraphics[width=4cm,height=4cm]{4638fg1a.ps} \in... ...1b.ps} }\\ \hspace*{1.8cm}{\bf (a)}\hspace*{4.0cm}{\bf (b)} \par\end{figure}$ Figure 1: H $_{\alpha }$ images acquired at the INAF-Catania Astrophysical Observatory on 15 April a) and 16 April b), 2002, at 07:39 and 07:03 UT, respectively. The arrow in the image on the left indicates the presence of a filament. The field of view is ${\sim }280 \times 280$ Mm². North is on the top and West on the right.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=3.8cm,height=3.8cm]{4638fg3a.ps}... ...8fg3d.ps} }\\ \hspace*{1.6cm}{\bf (c)}\hspace*{4.0cm}{\bf (d)} \end{figure}$ Figure 3: Sequence of TRACE images acquired at 195 $\AA$ , showing the evolution of an X-configuration in the loops, taking place before the flare peak. The field of view is ${\sim } 50 \times 50$ Mm².
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4638fig4.ps} \end{figure}$ Figure 4: Plot of the distance between the loop footpoints as a function of time. The solid line is the linear fit used to evaluate the footpoint distance growth speed.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{4638fig5.ps} \end{figure}$ Figure 5: RHESSI light curves of the M 2.5 flare occurred on 16 April 2002 in the 6-12 keV and in the 12-25 keV bands.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.9cm]{4638fg6a.ps} \includegrap... ...38fg6d.ps} }\\ \hspace*{2.0cm}{\bf (c)}\hspace*{5.cm}{\bf (d)} \end{figure}$ Figure 6: Sequence of RHESSI images analyzed with the CLEAN method. The dotted lines show the shape of the structure. It has an X configuration in the pre-flare phase and a Y configuration after the flare peak.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4cm,height=4cm]{4638fg1a.ps} \in... ...1b.ps} }\\ \hspace{1.8cm}{\bf (a)}\hspace{4.0cm}{\bf (b)} \par\end{figure}$	Figure 1: H $_{\alpha }$ images acquired at the INAF-Catania Astrophysical Observatory on 15 April a) and 16 April b), 2002, at 07:39 and 07:03 UT, respectively. The arrow in the image on the left indicates the presence of a filament. The field of view is ${\sim }280 \times 280$ Mm². North is on the top and West on the right.
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$\begin{figure} \par\mbox{\includegraphics[width=4cm,height=4cm]{4638fg2a.ps} \in... ...8fg2f.ps} }\\ \hspace{1.8cm}{\bf (e)}\hspace{4.0cm}{\bf (f)} \end{figure}$	Figure 2: Sequence of TRACE images acquired at 195 Å while the loops increase their brightness and assume a cusp shape. The field of view is ${\sim } 105 \times 105$ Mm².
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$\begin{figure} \par\mbox{\includegraphics[width=3.8cm,height=3.8cm]{4638fg3a.ps}... ...8fg3d.ps} }\\ \hspace{1.6cm}{\bf (c)}\hspace{4.0cm}{\bf (d)} \end{figure}$	Figure 3: Sequence of TRACE images acquired at 195 $\AA$ , showing the evolution of an X-configuration in the loops, taking place before the flare peak. The field of view is ${\sim } 50 \times 50$ Mm².
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4638fig4.ps} \end{figure}$	Figure 4: Plot of the distance between the loop footpoints as a function of time. The solid line is the linear fit used to evaluate the footpoint distance growth speed.
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$\begin{figure} \par\includegraphics[width=7cm]{4638fig5.ps} \end{figure}$	Figure 5: RHESSI light curves of the M 2.5 flare occurred on 16 April 2002 in the 6-12 keV and in the 12-25 keV bands.
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$\begin{figure} \par\mbox{\includegraphics[width=4.9cm]{4638fg6a.ps} \includegrap... ...38fg6d.ps} }\\ \hspace{2.0cm}{\bf (c)}\hspace{5.cm}{\bf (d)} \end{figure}$	Figure 6: Sequence of RHESSI images analyzed with the CLEAN method. The dotted lines show the shape of the structure. It has an X configuration in the pre-flare phase and a Y configuration after the flare peak.
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$\begin{figure} \par\includegraphics[width=7.8cm,]{4638fg7a.ps}\\ \hspace{3.7c... ...graphics[width=7.8cm,]{4638fg7b.ps}\\ \hspace{3.7cm}{\bf (b)} \end{figure}$	Figure 7: Plots of the loop height versus time a) in the 6-12 keV band and b) in the 12-25 keV band.
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