All Figures

$\begin{figure} \par\includegraphics[width=13.8cm]{fig1.eps}\end{figure}$ Figure 1: Clockwise from the upper left. Yohkoh/SXT images (3 November 1997, 14:17 UT, Al.1 filter): full disk image, active region including the CDS field of view, CDS field of view; magnetogram of the CDS field of view (courtesy of NSO/Kitt Peak). The CDS field of view is marked in the two upper images. Contours of the O V line data (raster 8) are superposed on the magnetogram. The letters in the magnetogram mark the position of the footpoints of loops A and B. The color scale of the magnetogram ranges from -280 G (deep red) to 470 G (deep blue).
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In the text

$\begin{figure} \par\includegraphics[width=10.9cm,clip]{h3483f2.eps}\end{figure}$ Figure 2: Top: sketch of the two loop structures identified in the CDS field of view. Bottom: two images of raster 8, clearly showing the two structures; left panel: the observation in the line of Fe XVI 360.76 Å; right panel: the one in the O V 629.73 Å line. The coordinates are in the heliocentric reference system. The gray scales are linear (for the extremes of the range see Fig. 3).
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In the text

$\begin{figure} \par\includegraphics[angle=180,width=14cm,clip]{h3483f3.eps}\end{figure}$ Figure 3: Second CDS raster of the observed region in several continuum-subtracted lines. The images are ordered with increasing line-formation-temperature. $\lambda_{\min}=l$ and $\lambda_{\max}=L$ are the extremes of the integration in wavelength (Å) for each picture, m and M are the extremes of the linear grey scale (photons s^-1 arcsec^-2 cm^-2).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{h3483f4.ps}\end{figure}$ Figure 4: Turn-on and -off of loop B in the O V 629 Å line, ( $\log T = 5.3$ ). Images are integrated in the band [628.69, 630.81] Å. Rasters are separated by 800 s. The upper left panel shows the entire loop at its maximum visibility (raster 8).
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In the text

$\begin{figure} \par\includegraphics[width=11.2cm,clip]{h3483f5.eps}\end{figure}$ Figure 5: Loop A: sectors chosen to obtain the brightness profiles. Images are from raster 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{h3483f6.eps}\end{figure}$ Figure 6: Loop A: normalized profiles of luminosity along the loop, at a single time (raster 3) and for several lines. X-axis: coordinate along the loop from NW footpoint to SE footpoint; Y-axis: average intensity normalized to the maximum. For clarity's sake, the profiles are separated by an offset equal to 0.5. The lines are ordered from the bottom up with increasing temperature of line formation.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{h3483f7.eps}\end{figure}$ Figure 7: Loop A: as in Fig. 6, but for all rasters and for three representative lines. For clarity's sake, the profiles are separated by an offset of 0.3.
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In the text

$\begin{figure} \par\includegraphics[width=10.5cm,clip]{fig8.ps}\end{figure}$ Figure 8: Loop A: profiles of luminosity along the loop in two CDS lines analogous to those shown in Fig. 7, but with no offset and no normalization (the units are kphot s^-1 cm^-2 arcsec^-2). Darker and darker lines correspond to progressively later times.
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In the text

$\begin{figure} \par\includegraphics[width=11.4cm,clip]{fig9.ps}\end{figure}$ Figure 9: The boxes in the images mark the zones for which we have generated the light curves; the zones include also the solid borders.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=11.2cm,clip]{fig10.ps}\end{figure}$ Figure 10: Light curves of the apex ( squares), SE footpoint ( triangles) and NW footpoint. In each diagram the horizontal solid line marks the noise level.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{fig11.ps}\end{figure}$ Figure 11: Emission Measure (EM) versus temperature for the hottest lines. The value obtained from Yohkoh data is also shown ( square).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{fig12.ps}\end{figure}$ Figure 12: Loop B: Gaussian fit of spectral data relative to the O V line, normalized to the maxima of the fitting functions at time of raster 7. Data and the fitting of the spectrum of the entire field of view ( diamonds and solid line, respectively) and of the S-W footpoint of the loop ( squares, dashed line) are shown.
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In the text

$\begin{figure} \par\includegraphics[width=10.9cm,clip]{h3483f2.eps}\end{figure}$	Figure 2: Top: sketch of the two loop structures identified in the CDS field of view. Bottom: two images of raster 8, clearly showing the two structures; left panel: the observation in the line of Fe XVI 360.76 Å; right panel: the one in the O V 629.73 Å line. The coordinates are in the heliocentric reference system. The gray scales are linear (for the extremes of the range see Fig. 3).
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$\begin{figure} \par\includegraphics[angle=180,width=14cm,clip]{h3483f3.eps}\end{figure}$	Figure 3: Second CDS raster of the observed region in several continuum-subtracted lines. The images are ordered with increasing line-formation-temperature. $\lambda_{\min}=l$ and $\lambda_{\max}=L$ are the extremes of the integration in wavelength (Å) for each picture, m and M are the extremes of the linear grey scale (photons s^-1 arcsec^-2 cm^-2).
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$\begin{figure} \par\includegraphics[angle=90,width=14cm,clip]{h3483f4.ps}\end{figure}$	Figure 4: Turn-on and -off of loop B in the O V 629 Å line, ( $\log T = 5.3$ ). Images are integrated in the band [628.69, 630.81] Å. Rasters are separated by 800 s. The upper left panel shows the entire loop at its maximum visibility (raster 8).
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$\begin{figure} \par\includegraphics[width=11.2cm,clip]{h3483f5.eps}\end{figure}$	Figure 5: Loop A: sectors chosen to obtain the brightness profiles. Images are from raster 1.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{h3483f7.eps}\end{figure}$	Figure 7: Loop A: as in Fig. 6, but for all rasters and for three representative lines. For clarity's sake, the profiles are separated by an offset of 0.3.
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$\begin{figure} \par\includegraphics[width=10.5cm,clip]{fig8.ps}\end{figure}$	Figure 8: Loop A: profiles of luminosity along the loop in two CDS lines analogous to those shown in Fig. 7, but with no offset and no normalization (the units are kphot s^-1 cm^-2 arcsec^-2). Darker and darker lines correspond to progressively later times.
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$\begin{figure} \par\includegraphics[width=11.4cm,clip]{fig9.ps}\end{figure}$	Figure 9: The boxes in the images mark the zones for which we have generated the light curves; the zones include also the solid borders.
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$\begin{figure} \par\includegraphics[angle=270,width=11.2cm,clip]{fig10.ps}\end{figure}$	Figure 10: Light curves of the apex ( squares), SE footpoint ( triangles) and NW footpoint. In each diagram the horizontal solid line marks the noise level.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{fig11.ps}\end{figure}$	Figure 11: Emission Measure (EM) versus temperature for the hottest lines. The value obtained from Yohkoh data is also shown ( square).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{fig12.ps}\end{figure}$	Figure 12: Loop B: Gaussian fit of spectral data relative to the O V line, normalized to the maxima of the fitting functions at time of raster 7. Data and the fitting of the spectrum of the entire field of view ( diamonds and solid line, respectively) and of the S-W footpoint of the loop ( squares, dashed line) are shown.
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