All Figures

$\begin{figure} \par\includegraphics[width=9cm,angle=0]{10049f1a.eps}\hspace*{2mm} \includegraphics[width=8.5cm,angle=0]{10049f1b.eps} \end{figure}$ Figure 1: Left: GOES soft X-ray flux curve at 02:50-04:20 UT, with flare class classification A-X. The dashed region indicates Yohkoh satellite night time, when no observations are available from the experiment. Plane-of-the-sky heliocentric CME front distances (boxes combined with a dotted line) are from the LASCO CME Catalog. Black boxes between 03:01:30 and 03:03:30 UT show the projected distances of the soft X-ray loop-like front, measured from the center of the eruption region at 1 $R_{\odot }$ . Right: detailed plot of the estimated distances/heights measured in the time interval 03:01:00-03:04:20 UT. Projected distances (km) from the eruption center are shown for the SXT loop-like front (stars/dash-dotted line) and the EUV ``blob'' (crosses/dotted line). The estimated type II burst heights are calculated with the 10 $\times$ Saito density model for the fragmented part (the three height-time data points, marked with diamonds, are from the start times of each three fragment. The type II heights for the later regular part (dashed lines) are calculated with the hybrid density model (corresponding to 5 $\times$ Saito) which describes a ``standard'' solar atmosphere. Applying a high-density model like 10 $\times$ Saito for the regular type II part at $\lesssim$ 130 MHz would imply at least streamer densities, see text for details. Yohkoh HXT hard X-ray counts in the 23-33 keV energy channel are also shown (bottom panel). Note that the drop in counts near 03:04 UT is due to the satellite entering night time.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{10049f2.eps} \end{figure}$ Figure 2: HiRAS dynamic spectrum from the 25-2500 MHz frequency range, at 03:00-03:10 UT on 13 May 2001. ``F'' notes emission at the fundamental and ``H'' at the second harmonic plasma frequency. Arrows point to the fragmented emission bands and dashed white lines outline the later-appearing ``regular'' type II burst lanes.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{10049f3.eps} \end{figure}$ Figure 3: Yohkoh SXT composite of images taken with two different filters and field of views at 02:54 UT on 13 May 2001. It shows the pre-eruption flare region and interconnecting loops. Axes are in arc seconds and white areas in the image mark saturated pixels.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{10049f4.eps} \end{figure}$ Figure 4: TRACE EUV image at 03:02:04 UT ( top), showing the erupting filament. Most of the filament material moved toward the Southeast (speed $\approx$ 380 km s^-1), but a blob-like structure moved more to the Southwest (speed $\approx$ 450 km s^-1). Arrows give the direction of motion for these structures. Yohkoh SXT image ( bottom) shows the same region in soft X-rays. The pointing for TRACE seems to be off from that of Yohkoh and so point-to point comparison is ambiguous.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{10049f5.eps} \end{figure}$ Figure 5: SXT difference images (AlMg filters) at 03:02:50 UT and 03:03:30 UT, showing the loop-like eruption front in soft X-rays. The later difference image is near the time of the appearance of the ``regular'' metric type II burst at 03:03:35 UT. The projected plane-of-the sky speed of the soft X-ray front is about 650 km s^-1 (arrows point to the loop front).
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In the text

$\begin{figure} {\bf\hspace{0.09\textwidth} \color{black} {Density} \hspace{0.0... ...idth} \color{black} {$x$ } \hfill } \vspace{-0.01\textwidth} \par\end{figure}$ Figure 6: The initial state of the simulation: density ( left half) and Alfvén speed ( right half). The white lines depict magnetic field lines. The units in the color bar are for the density (left values in the color bar) $1.67 \times 10^{-15} ~\mbox{ g~cm}^{-3}$ and for the Alfvén speed (right values in the color bar) $143 ~\mbox{ km~s}^{-1}$ , the isothermal sound speed. Note the clipping of the color bar; a brown color indicates values larger than the color bar maximum.
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In the text

$\begin{figure} \includegraphics[width=8cm,clip=]{10049f7.eps} \end{figure}$ Figure 7: The density ( left half) and speed ( right half) at three different times, t=220 a), t=270 b) and t=330 c) seconds. The white lines depict the magnetic field lines. The units in the color bar are for the density $1.67 \times 10^{-15} ~\mbox{ g~cm}^{-3}$ and for the speed $143 ~\mbox{ km~s}^{-1}$ . Note that both quantities are plotted using the same color bar.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{10049f8a.eps}\includegraphics[width=7.8cm,clip]{10049f8b.eps} \end{figure}$ Figure 8: Left: plot of the height-time data of the flux rope (solid line) and shock front (broken line) for the three simulation runs. Red corresponds to run A, blue to run B and green to run C. Right: plot of the corresponding flux rope and shock speed.
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In the text

$\begin{figure} {\includegraphics[width=7cm]{10049f9.eps} }\end{figure}$ Figure 9: Radio track of the three simulation runs. The size of the marker indicates the compression ratio of the shock.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{10049f2.eps} \end{figure}$	Figure 2: HiRAS dynamic spectrum from the 25-2500 MHz frequency range, at 03:00-03:10 UT on 13 May 2001. ``F'' notes emission at the fundamental and ``H'' at the second harmonic plasma frequency. Arrows point to the fragmented emission bands and dashed white lines outline the later-appearing ``regular'' type II burst lanes.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{10049f3.eps} \end{figure}$	Figure 3: Yohkoh SXT composite of images taken with two different filters and field of views at 02:54 UT on 13 May 2001. It shows the pre-eruption flare region and interconnecting loops. Axes are in arc seconds and white areas in the image mark saturated pixels.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{10049f5.eps} \end{figure}$	Figure 5: SXT difference images (AlMg filters) at 03:02:50 UT and 03:03:30 UT, showing the loop-like eruption front in soft X-rays. The later difference image is near the time of the appearance of the ``regular'' metric type II burst at 03:03:35 UT. The projected plane-of-the sky speed of the soft X-ray front is about 650 km s^-1 (arrows point to the loop front).
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$\begin{figure} \includegraphics[width=8cm,clip=]{10049f7.eps} \end{figure}$	Figure 7: The density ( left half) and speed ( right half) at three different times, t=220 a), t=270 b) and t=330 c) seconds. The white lines depict the magnetic field lines. The units in the color bar are for the density $1.67 \times 10^{-15} ~\mbox{ g~cm}^{-3}$ and for the speed $143 ~\mbox{ km~s}^{-1}$ . Note that both quantities are plotted using the same color bar.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{10049f8a.eps}\includegraphics[width=7.8cm,clip]{10049f8b.eps} \end{figure}$	Figure 8: Left: plot of the height-time data of the flux rope (solid line) and shock front (broken line) for the three simulation runs. Red corresponds to run A, blue to run B and green to run C. Right: plot of the corresponding flux rope and shock speed.
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$\begin{figure} {\includegraphics[width=7cm]{10049f9.eps} }\end{figure}$	Figure 9: Radio track of the three simulation runs. The size of the marker indicates the compression ratio of the shock.
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