All Figures

$\begin{figure} \par\includegraphics[width=14cm]{1378f1.eps} \end{figure}$ Figure 1: Yohkoh SXT images showing the X-ray connectivities on February 5, 6, and 8, 2000. The first two images show the complex loop structures, with possible coronal X-points and transequatorial loops connecting the two active regions NOAA 8858 and 8856. The last image on February 8 is post-flare and post-CME, when some of the loops have already disappeared.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{1378f2.eps} \end{figure}$ Figure 2: EUV images of the flare region: at the top: TRACE 171 Å images at 8:44:05, 8:46:53, 8:48:17, and 8:49:32 UT showing the westward moving fan-like structure (direction of movement shown with the white arrow). The speed of the moving fan was estimated to be around 100 km s^-1. The two separating flare ribbons are also visible. At the bottom: SOHO EIT difference image at 08:48-08:36 UT. EIT dimming regions correspond well to the decreased brightness areas in the TRACE images - i.e. areas uncovered by the moving fan. The TRACE field view is indicated by the box in the EIT difference image.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1378f2b.eps} \end{figure}$ Figure 3: SOHO MDI magnetogram from 08:03 UT shows the pre-flare multipolar active region. Yohkoh hard X-ray sources at 08:48:19 UT (HXT LO channel, 14-23 keV) are plotted over in white contours. The flare starts over a compact bipolar region, and hard X-rays are observed near the footpoints of a small X-ray loop. The TRACE field of view is indicated by the box.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{1378f3a.eps} \includegraphics[width=11.5cm,clip]{1378f3b.eps} \end{figure}$ Figure 4: At the top: times and positions of the EUV and soft X-ray (SXR) loops and waves, superposed on the EIT difference image at 08:48-08:36 UT. White arrow shows the direction of the EUV moving fan-like structure a), with estimated speed of 100 km s^-1. The first ejected SXR loop b), shown at 08:48:50 UT-08:49:22 UT (white lines) had an estimated projected speed between 220 and 520 km s^-1. The SXR expanding structure c), shown at 08:48:56-08:49:28 UT (black dashed lines) was estimated to have projected speed between 320 km s^-1 and 540 km s^-1. The front of the expanding SXR "bubble'' d), shown at 08:50:28 and 08:51:28 UT (black lines) had a projected speed around 720 km s^-1. The northwards moving SXR structure e), shown at 08:52:38 and 08:53:08 UT (white dashed lines) was estimated to have a projected speed around 120 km s^-1. At the bottom: the expanding SXR "bubble'' is shown at two selected time intervals, in rotated running difference images (Yohkoh SXT). Arrows indicate the expanding structures. The (projected) speeds were determined from positional changes (arcseconds on the disk) of the loop fronts over radials in the direction of the loop movements (different for each). No corrections were made for heights or changing line of sight.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{1378f4.eps} \end{figure}$ Figure 5: EIT difference images at 09:00-08:48 UT a) and at 10:00-08:36 UT b), Yohkoh SXT difference image at 10:00-08:33 UT c), and EIT difference image at 10:00-08:36 UT with overplotted contours of the SXT difference image from the same time d). The disappeared SXT and EIT transequatorial loops are indicated by arrows. It is evident that the footpoints of the dimmed loops connect to the same active regions.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1378f5.eps} \end{figure}$ Figure 6: At the top: radio spectra at the 40-800 MHz frequency range from OSRA/Tremsdorf at 08:40-09:08 UT. The different spectral parts in the composite image have been enhanced to show less intense emission in more detail. The radio type III bursts are marked in the spectra with boxes A-C: A and B are single reverse slope (RS) bursts around 08:44 and 08:46 UT. C is a group of J-type bursts around 08:49-08:50 UT. D is a group of narrow-band fluctuations around 08:52 UT. Radio type II emission at the fundamental (near 80 MHz) and second harmonic (near 160 MHz) are visible during 08:53-08:56 UT. Radio type IV continuum emission starts around 800 MHz at 08:51 UT, and the burst envelope drifts towards the lower frequecies. Some parts of the radio spectra are shown in detail in Fig. 7. In the middle: Yohkoh HXT flux curves in the 14-23 keV and 23-33 keV energy channels. At the bottom: GOES soft X-ray flux at 12.5-1.5 keV and at 25-3 keV.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{1378f6.eps} \end{figure}$ Figure 7: Artermis-IV dynamic spectra at 100-350 MHz during 08:48-08:56:30 UT, and a detail of the time derivative of the Artermis-IV intensity during the J-burst group at 08:48:30-08:50:30 UT. The times of the J-burst group (C), the narrow-band fluctuations (D), and the type II burst (at second harmonic) are marked on the plot. The black triangles indicate the times and frequencies of the locations of one of the J-burst branches, shown in Fig. 8b. The black box gives the time of one narrow band burst at 236 MHz, the multiple locations of which are shown in Fig. 8c. The white boxes in the spectra indicate the times of the type II burst locations shown in Fig. 8d, at 164 MHz. At the bottom Yohkoh HXT LO channel counts are shown for comparison.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1378f7.eps} \end{figure}$ Figure 8: a): The location of the first reverse slope (RS) bursts "A'' and "B'' at 8:44:20 and 8:46:05 UT ( $\bigcirc$ ). b): One of the radio type III J-bursts in the "C'' group, the emission locations are marked at 8:49:55 UT at 236 MHz, 8:50:02 UT at 164 MHz, at 8:50:04 UT at 236 MHz, and at 8:50:06 UT at 432 MHz ( $\vartriangle$ ), arrow shows the temporal evolution. The J-burst becomes visible first at 236 MHz and drifts towards the lower frequencies - the spectral turnover occurs around 140 MHz - and after that the burst drifts towards the higher frequencies, i.e. it goes down in the solar atmosphere. The frequencies and times were indicated with $\vartriangle$ in the dynamic spectra in Fig. 7. c): The three separate locations of the narrow-band burst at 8:52:04 UT at 236 MHz ( $\blacksquare$ ) belonging to the burst group "D''. d): Type II burst locations at 164 MHz at 08:53, 08:54, and 08:55 UT ( $\square$ ). Arrow shows the spatial movement in time, i.e. it first moves down and towards the inner part of the disk but then shifts slightly back towards the disk edge. The black arrow points to the bright region where the type II exiter is thought to collide with the active region belt/coronal streamer. The location of the stationary metric type IV emission is also indicated ( $\bullet$ ). All the radio sources are plotted over the EIT difference image at 9:00-8:48 UT. Dimming regions (depleted matter) are shown as dark regions, while bright regions represent more hot or dense matter.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=13cm,clip]{1378f8.eps} \end{figure}$ Figure 9: The start of the halo CME was observed by SOHO LASCO C2 at 09:30 UT over the North-East limb, and the location of the M 1.3 GOES flare in AR 8858 is also indicated in the image. The height-time plot from the LASCO CME Catalog is also shown. The estimated onset time of the CME depends on the fit and the number of fitted data points. The different types of radio burst sources are marked over an EIT difference image at 10:00-08:36 UT, which shows the deepest EUV dimmed regions on the solar disk: $\bigcirc$ RS bursts "A'' and "B''; $\vartriangle$ J-burst belonging to group "C''; $\blacksquare$ Narrow-band burst belonging to group "D''; $\square$ Type II burst; $\bullet$ Stationary metric type IV burst.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14cm]{1378f1.eps} \end{figure}$	Figure 1: Yohkoh SXT images showing the X-ray connectivities on February 5, 6, and 8, 2000. The first two images show the complex loop structures, with possible coronal X-points and transequatorial loops connecting the two active regions NOAA 8858 and 8856. The last image on February 8 is post-flare and post-CME, when some of the loops have already disappeared.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1378f2b.eps} \end{figure}$	Figure 3: SOHO MDI magnetogram from 08:03 UT shows the pre-flare multipolar active region. Yohkoh hard X-ray sources at 08:48:19 UT (HXT LO channel, 14-23 keV) are plotted over in white contours. The flare starts over a compact bipolar region, and hard X-rays are observed near the footpoints of a small X-ray loop. The TRACE field of view is indicated by the box.
Open with DEXTER