All Figures

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8575fig1.eps}\end{figure}$ Figure 1: a) Soft 1-8 Å X-ray flux obtained by GOES-10. b) Hard X-ray light curve from RHESSI, the energy band is 50-100 keV. c) Radio dynamic spectrum from WAVES/WIND. The frequency range is from 1.075 to 13.875 MHz. d) Radio dynamic spectrum from RSTN. The frequency range is from 25 to 180 MHz.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{8575fig2.eps}\end{figure}$ Figure 2: a) Trace 1600 Å image at 07:50:50 UT. b) Longitudinal magnetic map obtained by MDI onboard SOHO at 08:03:02 UT. The magnetic field scale is confined to -300 to 300 Gauss. The RHESSI HXR intensity image in 50-100 KeV energy band is co-aligned as red contour lines, the contour levels are 0.27, 0.4, 0.6 and 0.9 of maximum intensity.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{8575fig3.eps}\end{figure}$ Figure 3: a) EIT 195 Å intensity image at 07:50:59 UT. The location of the polar coronal hole is indicated as ``C'' and the boundary of the filament channel is indicated as ``B''. The white rectangle indicates the area which is indicated in Fig. 5. b)-d) EIT 195 Å base difference images at 08:01:23 UT, 08:12:04 UT and 08:23:53 UT, the image at 07:50:59 UT has been subtracted. The arrows ``e1-e2'' point to the footpoints of the loop-like eruptive features (in b) and c)), ``L'' indicates the well defined loop hanging out of the solar limb (in c) and ``fe'' is the extreme extent point of the diffuse emission enhancements on the boundary of the polar coronal hole (in d)).
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8575fig4.eps}\end{figure}$ Figure 4: Sequence of SXI running difference images. The eruptive features from the flare site are indicated by ``t1'', ``t2'' and ``t3''. The points indicated by ``f1-f4'' are the footpoints of the coronal bright signatures on the solar surface.
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In the text

$\begin{figure} \par\includegraphics[width=8.65cm,clip]{8575fig5.eps}\end{figure}$ Figure 5: a) The longitudinal magnetic field map at 08:03:02 UT, the magnetic field strengths are confined in -50 to 50 Gauss. b) EIT intensity image at 08:01:23 UT. c), d) EIT base difference images at 08:12:04 UT and 08:23:53 UT, the image at 07:50:59 UT has been subtracted. The points ``f1-f4'' are the same as indicated in Fig. 4 and ``e1-e2'' are the same as indicated in Fig. 3.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{8575fig6.eps}\end{figure}$ Figure 6: Distances of the footpoints of the brightening signatures from the flare site. The black arrow shows the onset time of metric radio bursts.
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In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8575fig1.eps}\end{figure}$	Figure 1: a) Soft 1-8 Å X-ray flux obtained by GOES-10. b) Hard X-ray light curve from RHESSI, the energy band is 50-100 keV. c) Radio dynamic spectrum from WAVES/WIND. The frequency range is from 1.075 to 13.875 MHz. d) Radio dynamic spectrum from RSTN. The frequency range is from 25 to 180 MHz.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{8575fig2.eps}\end{figure}$	Figure 2: a) Trace 1600 Å image at 07:50:50 UT. b) Longitudinal magnetic map obtained by MDI onboard SOHO at 08:03:02 UT. The magnetic field scale is confined to -300 to 300 Gauss. The RHESSI HXR intensity image in 50-100 KeV energy band is co-aligned as red contour lines, the contour levels are 0.27, 0.4, 0.6 and 0.9 of maximum intensity.
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$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8575fig4.eps}\end{figure}$	Figure 4: Sequence of SXI running difference images. The eruptive features from the flare site are indicated by ``t1'', ``t2'' and ``t3''. The points indicated by ``f1-f4'' are the footpoints of the coronal bright signatures on the solar surface.
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$\begin{figure} \par\includegraphics[width=8.65cm,clip]{8575fig5.eps}\end{figure}$	Figure 5: a) The longitudinal magnetic field map at 08:03:02 UT, the magnetic field strengths are confined in -50 to 50 Gauss. b) EIT intensity image at 08:01:23 UT. c), d) EIT base difference images at 08:12:04 UT and 08:23:53 UT, the image at 07:50:59 UT has been subtracted. The points ``f1-f4'' are the same as indicated in Fig. 4 and ``e1-e2'' are the same as indicated in Fig. 3.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{8575fig6.eps}\end{figure}$	Figure 6: Distances of the footpoints of the brightening signatures from the flare site. The black arrow shows the onset time of metric radio bursts.
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