All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig1} \end{figure}$ Figure 1: MDI image showing the position of active regions on October 14, 1999. An impulsive X1/1N flare occured in region 8371 at 0858 UT.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig2} \end{figure}$ Figure 2: Series of images built from the H $\alpha$ information showing the filament eruption. The dark regions correspond to blueshifted (rising) features, while the bright regions correspond to redshifted (falling) features. As we can see the material is rising while moving outward in the first frames, but later on, after 0920 UT we see evidence for inward motion of material falling back.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig3} \end{figure}$ Figure 3: Running difference images in H $\alpha$ showing the progression of a Moreton wave indicated by the arrows.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig4} \end{figure}$ Figure 4: Position of the main radio emitting regions A, B, C, D, E and F. Different symbols correspond to different observing frequencies: squares to 164 MHz, triangles to 236 MHz, crosses to 327 MHz and circles to 410 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig5} \end{figure}$ Figure 5: Flux versus time of the event at the different observing frequencies of the NRH. After a relatively quiet period with only weak bursts at low frequencies, the flux raises by a few orders of magnitude shortly after 08:58 UT. This outburst that lasts a few minutes is then followed by relatively stable or low rising continua at the different frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig6} \end{figure}$ Figure 6: Composite spectrum in the band of 1 MHz-7.6 GHz, observated by Wind/Waves (1-10 MHz), Porto (150-650 MHz), Ondrejov (0.8-4.5 GHz) and Beijing (5.2-7.6 GHz).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig7} \end{figure}$ Figure 7: Peak brightness temperature time at 410 for small boxes encompassing sources A and D. The only relevant outbursts are seen a few seconds after 0858 UT, nearly simultaneous at the two positions (brightness at D starts rising some 20 to 30 s later than at A).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig8} \end{figure}$ Figure 8: (From the top) Panel 1: flux evolution of sources C at 236 MHz. Panels 2 and 3: flux evolution of sources D and E at 164 MHz and 327 MHz. The broad band continuum is associated with D and the bursty emission with E.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig9} \end{figure}$ Figure 9: Flux and location evolution of source F. At about 08:58:30 a new source is seen in radio images at 164 MHz. This source shows a displacement toward the north with an apparent speed about 6000 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig10} \end{figure}$ Figure 10: After 08:59:23 UT the D source becomes extremely elongated in the direction shown by the line in the 410 MHz image in the upper right corner. The brightness profiles taken along this line show an excess brightness that moves with an apparent velocity about 1500 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig11} \end{figure}$ Figure 11: LASCO images of the CME showing its progression. A series of key figures are indicated in the C2 image at 0926:05 UT. The arrow in C3 images indicates a feature that seems to correspond to K3 that expands at a different rate to the rest of the CME.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig12} \end{figure}$ Figure 12: Height-time plot for features K1 and K3 in the CME.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig13} \end{figure}$ Figure 13: Decelerated CME? The circle indicated by the arrow shows the extrapolated position of the CME leading edge at this time. No evidence for the CME is seen in the LASCO image.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{ms3118-fig14} \end{figure}$ Figure 14: Left: Yohkoh/SXT image of the active complex (12:42 UT) superimposed with the position of the radio sources observed with the NRH. Right: Same SXT image overlaid by magnetic field lines calculated from the linear force-free field extrapolation of the SOHO/MDI magnetogram (08:00 UT). The thin parallelogram shows a portion only of the magnetogram used for the extrapolation. Units are in arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{ms3118-fig15.eps.newRGB} \end{figure}$ Figure 15: Top left: SOHO/MDI magnetogram (grey levels) overlaid with the positions of observed radio sources (yellow) and some calculated magnetic field lines. Pink/blue contours stand for $B_z(z=0) = \pm 25,75,150,500,800$ G. The black field lines pass through the radio sources C, E, F. The cyan/yellow/red field lines surround the sepatrices of three nulls points located at low altitude (resp. at $z \simeq 6,4,5$ Mm) in the West part of the active complex. The green field lines surround the separatrix of a coronal null point located in the vicinity of the flare region at $z \simeq 26$ Mm. Top right: same plot showing the field lines in projection from the North-West. Bottom left: zoom with same projection on the coronal null point, with a vertical stretching factor of 2.5. Bottom right: zoom with same projection on the low altitude null points. Units are in arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig1} \end{figure}$	Figure 1: MDI image showing the position of active regions on October 14, 1999. An impulsive X1/1N flare occured in region 8371 at 0858 UT.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig2} \end{figure}$	Figure 2: Series of images built from the H $\alpha$ information showing the filament eruption. The dark regions correspond to blueshifted (rising) features, while the bright regions correspond to redshifted (falling) features. As we can see the material is rising while moving outward in the first frames, but later on, after 0920 UT we see evidence for inward motion of material falling back.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig3} \end{figure}$	Figure 3: Running difference images in H $\alpha$ showing the progression of a Moreton wave indicated by the arrows.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig4} \end{figure}$	Figure 4: Position of the main radio emitting regions A, B, C, D, E and F. Different symbols correspond to different observing frequencies: squares to 164 MHz, triangles to 236 MHz, crosses to 327 MHz and circles to 410 MHz.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig5} \end{figure}$	Figure 5: Flux versus time of the event at the different observing frequencies of the NRH. After a relatively quiet period with only weak bursts at low frequencies, the flux raises by a few orders of magnitude shortly after 08:58 UT. This outburst that lasts a few minutes is then followed by relatively stable or low rising continua at the different frequencies.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig6} \end{figure}$	Figure 6: Composite spectrum in the band of 1 MHz-7.6 GHz, observated by Wind/Waves (1-10 MHz), Porto (150-650 MHz), Ondrejov (0.8-4.5 GHz) and Beijing (5.2-7.6 GHz).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig7} \end{figure}$	Figure 7: Peak brightness temperature time at 410 for small boxes encompassing sources A and D. The only relevant outbursts are seen a few seconds after 0858 UT, nearly simultaneous at the two positions (brightness at D starts rising some 20 to 30 s later than at A).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig8} \end{figure}$	Figure 8: (From the top) Panel 1: flux evolution of sources C at 236 MHz. Panels 2 and 3: flux evolution of sources D and E at 164 MHz and 327 MHz. The broad band continuum is associated with D and the bursty emission with E.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig9} \end{figure}$	Figure 9: Flux and location evolution of source F. At about 08:58:30 a new source is seen in radio images at 164 MHz. This source shows a displacement toward the north with an apparent speed about 6000 km s^-1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig10} \end{figure}$	Figure 10: After 08:59:23 UT the D source becomes extremely elongated in the direction shown by the line in the 410 MHz image in the upper right corner. The brightness profiles taken along this line show an excess brightness that moves with an apparent velocity about 1500 km s^-1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig11} \end{figure}$	Figure 11: LASCO images of the CME showing its progression. A series of key figures are indicated in the C2 image at 0926:05 UT. The arrow in C3 images indicates a feature that seems to correspond to K3 that expands at a different rate to the rest of the CME.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig12} \end{figure}$	Figure 12: Height-time plot for features K1 and K3 in the CME.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{ms3118-fig13} \end{figure}$	Figure 13: Decelerated CME? The circle indicated by the arrow shows the extrapolated position of the CME leading edge at this time. No evidence for the CME is seen in the LASCO image.
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