All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,height=7.4cm,clip]{0666fg1a.eps}... ...mm} \includegraphics[width=7.7cm,height=7.4cm,clip]{0666fg1b.eps} \end{figure}$ Figure 1: BP2 location and semblance. Left image: context EIT Fe XII 195 Å full disk image (8 November 2002, 00:36 UT) with an arrow highlighting the location of the BP. Top right images: comparison of a close-up of the feature in EIT and TRACE Fe IX/X 171 Å taken 2 min earlier. Bottom right: magnetic field contours ( $\pm$ 25 G, solid/dotted contours) overlaying the TRACE image. The arcade of loops resolved by TRACE connects opposite polarities.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0666fg2.eps} \end{figure}$ Figure 2: Flux distribution for several EIT images of the same region, with no bright point (dashed lines) and with its presence (solid lines). The dotted line represents the threshold value chosen to define the BP.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.4cm,clip]{0666fg3.eps} \end{figure}$ Figure 3: Sample spectrum of the wide spectral window extracted from NIS 1 in one of the studies. The dotted lines represent the two fits used to subtract the continuum from the spectral lines. Some of the relevant ones are labeled.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.4cm,clip]{0666fg4a.eps}\hspace*{5mm} \includegraphics[angle=90,width=8.3cm,clip]{0666fg4b.eps} \end{figure}$ Figure 4: In the left panels are Mg IX 368, O V 629 and He I 584 rasters for the BP of 7 November 2002 (BP2). The slit location for the spectral data is highlighted by a dashed line and a solid contour shows the 3 $\sigma$ level. On the right hand panels, the plots correspond to the intensity profile along the dashed line in the raster. The dot-dashed line is the threshold level and the dotted lines delimit the interval of integration.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0666fg5.eps} \end{figure}$ Figure 5: Evolution in time of the EIT flux, magnetic flux and EIT flux per unit area (pixel) of the two consecutive BPs observed at the same location. Dashed lines delimit their lifetime. The observed data-points are represented by plus symbols, triangles represent times with simultaneous EIT and MDI data for BP1 and stars for BP2. The black dots are three points to be referred to in Fig. 6. The starting time is November 4, 2002, 00:00 UT.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0666fg6.eps} \end{figure}$ Figure 6: Relation between the EIT Fe XII flux and the magnetic flux. Same symbols as in Fig. 5 are used. The dashed line is the linear fit to the BP1 points (triangles) excluding the three black dots, and the dot-dashed line is the fit to the BP2 points (stars).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{0666fg7.eps} \end{figure}$ Figure 7: Flux variations for BP2 as seen in Mg IX, O V, O III and He I. Start time is November 7 at 16:20 UT. The three sections correspond to studies s26195, s26197 and s26199. Gaps in between were covered by context rasters. Dotted lines signal when the tracking correction took place. The formation temperature of the spectral line is provided beside its identification.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0666fg8a.eps}\hspace*{5mm} \includegraphics[width=8.6cm,clip]{0666fg8b.eps} \end{figure}$ Figure 8: BP2 wavelet results corresponding to study s26197 (middle series in Fig. 7) for O V 629.73 Å ( left) and He I 584.34 Å ( right). Top: detrended intensity in photon-events; center: wavelet power spectrum and global wavelet spectrum; bottom: level of probability for the two highest peaks in the spectrum. 1st maximums: thick dots and solid line; 2nd maximums: thin dots and dotted line. The dash-dotted line corresponds to a probability level of 95%. Start time is November 7, 2002 at 18:47 UT. The dashed line of the global wavelet plot represents the maximum period outside the COI.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0666fg9.eps} \end{figure}$ Figure 9: Damped oscillation observed in the O V 629 time series, study s26197. Overplotted in dot-dashed line there is an exponential damped sine function with a period of 546 s.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0666fg10.eps} \end{figure}$ Figure 10: Wavelet results for the SUMER BP. See caption in Fig. 8 for details. Units for the intensity are counts.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{0666fg11.eps} \end{figure}$ Figure 11: S VI detrended intensity fluctuations (solid line) corresponding to the SUMER BP. Overplotted with a dashed line there is a 491 s. period sinusoidal function.
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In the text

$\begin{figure} \par\mbox{\hspace*{2mm}\includegraphics[width=7.6cm,clip]{0666f12... ... \par\vspace*{5mm} \includegraphics[width=8cm,clip]{0666f12b.eps} \end{figure}$ Figure 12: Top figure: intensity changes along time for the two O IV lines that form the electron density sensitive ratio 625.8/608.4. Bottom figure: electron density changes along time. The start time is the same as in Fig. 7. The dotted lines serve as reference for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0666fg2.eps} \end{figure}$	Figure 2: Flux distribution for several EIT images of the same region, with no bright point (dashed lines) and with its presence (solid lines). The dotted line represents the threshold value chosen to define the BP.
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$\begin{figure} \par\includegraphics[angle=90,width=17.4cm,clip]{0666fg3.eps} \end{figure}$	Figure 3: Sample spectrum of the wide spectral window extracted from NIS 1 in one of the studies. The dotted lines represent the two fits used to subtract the continuum from the spectral lines. Some of the relevant ones are labeled.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0666fg6.eps} \end{figure}$	Figure 6: Relation between the EIT Fe XII flux and the magnetic flux. Same symbols as in Fig. 5 are used. The dashed line is the linear fit to the BP1 points (triangles) excluding the three black dots, and the dot-dashed line is the fit to the BP2 points (stars).
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$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{0666fg7.eps} \end{figure}$	Figure 7: Flux variations for BP2 as seen in Mg IX, O V, O III and He I. Start time is November 7 at 16:20 UT. The three sections correspond to studies s26195, s26197 and s26199. Gaps in between were covered by context rasters. Dotted lines signal when the tracking correction took place. The formation temperature of the spectral line is provided beside its identification.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0666fg9.eps} \end{figure}$	Figure 9: Damped oscillation observed in the O V 629 time series, study s26197. Overplotted in dot-dashed line there is an exponential damped sine function with a period of 546 s.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0666fg10.eps} \end{figure}$	Figure 10: Wavelet results for the SUMER BP. See caption in Fig. 8 for details. Units for the intensity are counts.
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$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{0666fg11.eps} \end{figure}$	Figure 11: S VI detrended intensity fluctuations (solid line) corresponding to the SUMER BP. Overplotted with a dashed line there is a 491 s. period sinusoidal function.
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$\begin{figure} \par\mbox{\hspace{2mm}\includegraphics[width=7.6cm,clip]{0666f12... ... \par\vspace{5mm} \includegraphics[width=8cm,clip]{0666f12b.eps} \end{figure}$	Figure 12: Top figure: intensity changes along time for the two O IV lines that form the electron density sensitive ratio 625.8/608.4. Bottom figure: electron density changes along time. The start time is the same as in Fig. 7. The dotted lines serve as reference for comparison.
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