All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1079fi1t.eps}\par\vspace*{... ...m}\includegraphics[width=6.8cm,clip]{1079fi1b.eps}\hspace*{1cm}} \end{figure}$ Figure 1: SXT full disc image at the time of maximum extension of the sigmoidal X-ray bright point ( top) and the closest in time MDI magnetogram ( bottom). The bright point is associated to a very small AR located at disc centre (both shown within the tiny boxes), which is very far from other ARs.
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In the text

$\begin{figure} \par\hspace*{2mm}\includegraphics[width=7.6cm,clip]{1079fi2t.eps}\par\vspace*{3mm} \includegraphics[width=7.9cm,clip]{1079fi2b.eps} \end{figure}$ Figure 2: Magnetic ( top) and X-ray flux evolution ( bottom) from the emergence to the disappearance of the small active region. The positive (negative) magnetic flux is shown with continuous (dashed) line. There are three main bursts in X-rays (marked with arrows in the bottom figure), which all occurred on May 11: the first at $\sim$ 01:00 UT, the second at $\sim$ 07:00 UT, and the third at $\sim$ 09:00 UT.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,height=18cm,clip]{1079fi3.eps} \end{figure}$ Figure 3: Photospheric magnetograms from SOHO/MDI showing the full evolution of the bright point region from May 10 to 12, 1998. The field of view is $200 \times 200$ arcsec (1.98 arcsec per pixel), the maps have been coaligned and derotated to central meridian position (11 May 04:15 UT).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,height=18cm,clip]{1079fi4.eps} \end{figure}$ Figure 4: Coronal evolution as seen in EUV with the SOHO/EIT (same field of view and treatment as in Fig. 3, 2.62 arcsec per pixel). All the images shown here are taken with the 284 Å filter, except the one on 11 May at 11:08 UT where the wavelength is 195 Å.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{1079fi5.eps} \end{figure}$ Figure 5: EIT 195 Å images in contrast-enhanced reversed colors (enhanced emission in black, reduced in white) of the bright point during the first and third X-ray bursts indicated in Fig. 2, bottom. The field of view is $150 \times 135$ arcsec in all images. However, because during the first burst the dimming stretches northward and during the third burst it does it southward, we have centered differently the top and bottom row images. The x axis runs from -100 (-25) to 50 (125) arcsec, while the y axis runs from 0 (-25) to 135 (110) arcsec, for the top ( bottom) row images.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1079fi6.eps} \end{figure}$ Figure 6: Top: difference images from EIT 195 Å at 08:48-08:31 UT showing the extension of the dimmings after the event starting after 08:03 UT (see Fig. 2, bottom). Bottom: MDI high resolution magnetogram closest in time with the overlaid contour of the dimmings. We have separated the dimmings North-East and South-West of the bipole and for each the extension above the small AR (continuous white/black lines on the negative/positive polarity) from that above the quiet Sun (dashed lines). Both images are $200 \times 200$ arcsec in size.
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In the text

$\begin{figure} \par\hspace{0cm} \includegraphics[width=8cm,clip]{1079fi7t.eps}\par\vspace*{3mm} \includegraphics[width=8cm,clip]{1079fi7b.eps} \end{figure}$ Figure 7: Flux, in units of 10¹⁹ Mx, measured in the dimmings in the quiet Sun (so, excluding the portion overlying the small AR, see the dashed lines shown in Fig. 6). Positive and negative field values are summed up separately and represented with continuous and dashed lines, respectively. Low magnetic flux densities are mostly due to noise or low scale magnetic connectivities. To derive the large scale flux only, the magnetic flux densities are filtered using a minimum threshold value.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1079fi8t.ps}\par\vspace*{3mm} \includegraphics[width=8.5cm,clip]{1079fi8b.ps} \end{figure}$ Figure 8: Top: TRACE 195 Å observation at 00:38 UT on May 11 (reversed color) with two isocontours (grey lines) of the photospheric field taken with MDI at 00:03 UT (positive: continuous, negative: dashed). Bottom: the same image with more isocontours ( $\pm$ 25, 50, 75, 100, 150, 200, grey lines) and computed field lines superimposed (the thin lines have been computed using $\alpha = -0.08$ Mm^-1 and the thick lines using $\alpha = -0.11$ Mm^-1). Notice the global S shape of the emission, which is a consequence of the strong non-potentiality of the magnetic field configuration. Both x and y axes are measured in Mm.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1079fi9t.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{1079fi9b.ps} \end{figure}$ Figure 9: Interplanetary magnetic field data obtained by the Wind spacecraft. The two upper panels show the complex ejecta (with the small MC located in between the dashed lines), and the three lower panels are a zoom on the small MC. We plot the magnetic field intensity (|B|) and its components in Geocentric Solar Ecliptic (GSE) coordinates as a function of time.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip=]{1079f10t.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip=]{1079f10b.ps} \par\end{figure}$ Figure 10: Magnetic field components in local MC coordinates. The two upper panels show the hodograms for the MC. The central and lower panels show the evolution of the magnetic field components (with the orientation of the cloud given by the minimum variance method, see Sect. 4.2). The observed magnetic data are drawn with thick lines, and the best solutions fitted using Lundquist's model are shown with thin lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1079f11.eps} \end{figure}$ Figure 11: Schematic global view of the magnetic cloud and its source region (notice that in this figure the solar North is to the left). The MC leading part is represented by continuous lines, while dashed lines are used closer to the Sun since, considering the photospheric magnetic observations, the MC should be detached from its solar source by the time it was observed by the Wind spacecraft.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip=]{1079f12t.eps}\par\vspace*{3mm} \includegraphics[width=7cm,clip=]{1079f12b.eps} \end{figure}$ Figure 12: A sketch showing the way a magnetic flux tube can be formed by magnetic reconnection in an expanding sheared arcade (Démoulin et al. 1996). The upper and lower figures show two field lines belonging to the expanding arcade ( top), and a small arcade and flux tube ( bottom), before and after reconnection respectively. PIL indicates the photospheric inversion line. Further reconnection between the flux tube and the large scale arcade will increase the number of turns in the flux tube. Coronal dimmings are expected to form in all the expanding arcade. However, only a fraction of the photospheric flux of the dimmings contributes to the longitudinal flux of the twisted flux tube; the remaining part is transferred (through reconnection) to the magnetic flux in the azimuthal component.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1079f13.ps} \end{figure}$ Figure 13: Comparison to the event studied by Manoharan et al. (1996). The left (resp. right) column correspond to X-ray images at the beginning (resp. after) the eruption. The top row shows the studied X-ray bright point, as observed in SXT full disc images (the field of view is about $80 \times 80$ arcsec). The middle and bottom rows are the SXT partial frame images of the event studied by Manoharan et al. (the field of view is about $310 \times 310$ arcsec). The original images are shown in the bottom row, while their spatial resolution has been degraded (rebinned) by a factor 8 in the middle row (to account both for the difference in the observed resolution, a factor 2, and spatial extension of the ARs, about a factor 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1079fi1t.eps}\par\vspace{... ...m}\includegraphics[width=6.8cm,clip]{1079fi1b.eps}\hspace{1cm}} \end{figure}$	Figure 1: SXT full disc image at the time of maximum extension of the sigmoidal X-ray bright point ( top) and the closest in time MDI magnetogram ( bottom). The bright point is associated to a very small AR located at disc centre (both shown within the tiny boxes), which is very far from other ARs.
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$\begin{figure} \par\includegraphics[width=7.5cm,height=18cm,clip]{1079fi3.eps} \end{figure}$	Figure 3: Photospheric magnetograms from SOHO/MDI showing the full evolution of the bright point region from May 10 to 12, 1998. The field of view is $200 \times 200$ arcsec (1.98 arcsec per pixel), the maps have been coaligned and derotated to central meridian position (11 May 04:15 UT).
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$\begin{figure} \par\includegraphics[width=7.5cm,height=18cm,clip]{1079fi4.eps} \end{figure}$	Figure 4: Coronal evolution as seen in EUV with the SOHO/EIT (same field of view and treatment as in Fig. 3, 2.62 arcsec per pixel). All the images shown here are taken with the 284 Å filter, except the one on 11 May at 11:08 UT where the wavelength is 195 Å.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1079fi9t.ps}\par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{1079fi9b.ps} \end{figure}$	Figure 9: Interplanetary magnetic field data obtained by the Wind spacecraft. The two upper panels show the complex ejecta (with the small MC located in between the dashed lines), and the three lower panels are a zoom on the small MC. We plot the magnetic field intensity (\|B\|) and its components in Geocentric Solar Ecliptic (GSE) coordinates as a function of time.
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