All Figures

$\begin{figure} \par\includegraphics[width=8cm]{2321fig1.eps} \end{figure}$ Figure 1: The GOES light curve for the 16th April 2002. The event studied in this paper occurred at around 12:50 UT.
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In the text

$\begin{figure} \par\includegraphics[width=15cm]{2321fig2.ps} \end{figure}$ Figure 2: A time series of TRACE 195 Å images. It clearly shows the formation of the flaring arcade with the formation of a cusp towards the end.
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In the text

$\begin{figure} \par\includegraphics[width=13cm]{2321fig3.ps} \end{figure}$ Figure 3: TRACE 195 Å images, with a reverse colour table. The field of view has been reduced to give a much clearer view of the lifting flux rope. The images are a time series from top left to bottom right. The lifting flux rope is seen as the dark feature expanding towards the right.
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In the text

$\begin{figure} \par\includegraphics[width=5.3cm,clip]{2321fi4a.eps}\includegraph... ...clip]{2321fi4b.eps}\includegraphics[width=5.3cm,clip]{2321fi4c.eps} \end{figure}$ Figure 4: Left: TRACE 195 Å image with a line illustrating the position of the CDS slit. Centre: CDS time series of slit intensity images. CDS was in a "sit and stare'' mode and this image shows what happened beneath the slit over the time of event. The crescent shape to the left of this image represents the lifting flux rope. Right: here we see the Dopplergram of the same data. The colour bar indicates the Doppler velocity where white is blue-shifted and black is red-shifted.
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In the text

$\begin{figure} \par\hspace{-0.3cm} \includegraphics[width=8.33cm,clip]{2321fi5a.... ...1cm} \includegraphics[width=7.9cm,height=4.5cm,clip]{2321fi5b.eps} \end{figure}$ Figure 5: Top: height-time plot for the lifting flux rope as seen by TRACE. The cross represents the leading edge of the flux rope as seen by CDS. Below the best-fit lines are the data points from the coronal hard X-ray source. Bottom: the hard X-ray light curve including all data between 5 and 50 keV over the same time frame as the height-time plot above.
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In the text

$\begin{figure} \par\hbox{ \psfig{figure=2321fi6a.eps,width=6cm}\psfig{figure=232... ...ure=2321fi6h.eps,width=6cm}\psfig{figure=2321fi6i.eps,width=6cm} }\end{figure}$ Figure 6: The images in this figure are all TRACE 195 Å images. On these images are RHESSI contours at 80%, 60%, 40%, 20% and 10% of the peak intensity. The top row shows contours from the 5-10 keV, the second row shows 10-15 keV and the final row has 15-20 keV contours. Of particular note is the coronal source. One can see that this source moves with time from left to right, i.e. upward.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2321fig7.ps}\end{figure}$ Figure 7: This height-time plot is derived from the coronal HXR source over three separate energy bands.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2321fi8a.eps}\par\includegraphics[width=6cm,clip]{2321fi8b.eps} \end{figure}$ Figure 8: The top light curve is constructed to show how the number of counts changes with time for the loop top source and the loop footpoints. They have been grouped together as it is very difficult to distinguish between them accurately. The bottom light curve is that of the coronal X-ray source located above loop top source.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2321fig9.eps} \end{figure}$ Figure 9: A synthetic slit image assembled from the TRACE data cube, designed to mimic the intensity data gathered from CDS.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{2321fi10.ps} \end{figure}$ Figure 10: A time series of MDI magnetograms, rotated to central meridian position in the days running up to the event on 16th April 2002. One can see the evolution of the region from the top left to the bottom right where projection effects distort the image dramatically. In the image from 14th April a box is drawn representing the region used in the extrapolations of Fig.11.
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In the text

$\begin{figure} \par\hbox{ \subfigure[]{\psfig{figure=2321f11a.ps,width=5.5cm,cli... ...=} } \subfigure[]{\psfig{figure=2321f11c.ps,height=5.5cm,clip=} }}\end{figure}$ Figure 11: a) Magnetic field lines extrapolated (local field of view, as if the AR is located at disk centre) in the linear force-free approximation ( $\alpha =0.015$ Mm^-1) using a SOHO/MDI full-disc magnetic map as boundary condition two days prior to the event. b) As in a) in a different point of view to enable one to see the arcade orientation. c) As in a) with the AR rotated to the time of the event. The axes are measured in Mm and the field of view extends from 290'' to 428'' in the North-South direction and from 838'' to 977'' in the East-West direction (see Fig. 2). The isocontour values are $\pm$ 100, 500, 1000 G.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2321fi12.ps} \end{figure}$ Figure 12: LASCO C2 difference image of the CME on 16th April 2002 at 13:50 UT, where the CME can be seen emerging from the occulting disk in the northwest.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2321fi13.ps} \end{figure}$ Figure 13: Height-time plot for the lifting flux rope as seen by TRACE and LASCO C2, with three different types of fit. The crosses represent the leading and trailing edge of the LASCO CME. We have an exponential growth, which can be seen to meet the required height in the required time. Then there is the polynomial fit and the linear fit which can never reach the required heights.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2321f14a.eps}\par\includeg... ...2321f14b.eps}\par\includegraphics[width=8cm,clip]{2321f14c.eps}\par \end{figure}$ Figure 14: Height-time plot for the lifting flux rope as seen by TRACE and LASCO C2 with error bars representing five pixels. The dashed line represents the continuation of the exponential fit to the TRACE data. This is followed by the velocity profile and acceleration profile derived from the first and second derivative of the fits to the data.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2321fi15.ps}\end{figure}$ Figure 15: Cartoon representing the entire event, based upon our observations from all instruments.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{2321fig1.eps} \end{figure}$	Figure 1: The GOES light curve for the 16th April 2002. The event studied in this paper occurred at around 12:50 UT.
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$\begin{figure} \par\includegraphics[width=15cm]{2321fig2.ps} \end{figure}$	Figure 2: A time series of TRACE 195 Å images. It clearly shows the formation of the flaring arcade with the formation of a cusp towards the end.
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$\begin{figure} \par\includegraphics[width=13cm]{2321fig3.ps} \end{figure}$	Figure 3: TRACE 195 Å images, with a reverse colour table. The field of view has been reduced to give a much clearer view of the lifting flux rope. The images are a time series from top left to bottom right. The lifting flux rope is seen as the dark feature expanding towards the right.
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$\begin{figure} \par\hspace{-0.3cm} \includegraphics[width=8.33cm,clip]{2321fi5a.... ...1cm} \includegraphics[width=7.9cm,height=4.5cm,clip]{2321fi5b.eps} \end{figure}$	Figure 5: Top: height-time plot for the lifting flux rope as seen by TRACE. The cross represents the leading edge of the flux rope as seen by CDS. Below the best-fit lines are the data points from the coronal hard X-ray source. Bottom: the hard X-ray light curve including all data between 5 and 50 keV over the same time frame as the height-time plot above.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2321fig7.ps}\end{figure}$	Figure 7: This height-time plot is derived from the coronal HXR source over three separate energy bands.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2321fi8a.eps}\par\includegraphics[width=6cm,clip]{2321fi8b.eps} \end{figure}$	Figure 8: The top light curve is constructed to show how the number of counts changes with time for the loop top source and the loop footpoints. They have been grouped together as it is very difficult to distinguish between them accurately. The bottom light curve is that of the coronal X-ray source located above loop top source.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2321fig9.eps} \end{figure}$	Figure 9: A synthetic slit image assembled from the TRACE data cube, designed to mimic the intensity data gathered from CDS.
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$\begin{figure} \par\includegraphics[width=14.5cm,clip]{2321fi10.ps} \end{figure}$	Figure 10: A time series of MDI magnetograms, rotated to central meridian position in the days running up to the event on 16th April 2002. One can see the evolution of the region from the top left to the bottom right where projection effects distort the image dramatically. In the image from 14th April a box is drawn representing the region used in the extrapolations of Fig.11.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2321fi12.ps} \end{figure}$	Figure 12: LASCO C2 difference image of the CME on 16th April 2002 at 13:50 UT, where the CME can be seen emerging from the occulting disk in the northwest.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2321fi13.ps} \end{figure}$	Figure 13: Height-time plot for the lifting flux rope as seen by TRACE and LASCO C2, with three different types of fit. The crosses represent the leading and trailing edge of the LASCO CME. We have an exponential growth, which can be seen to meet the required height in the required time. Then there is the polynomial fit and the linear fit which can never reach the required heights.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2321f14a.eps}\par\includeg... ...2321f14b.eps}\par\includegraphics[width=8cm,clip]{2321f14c.eps}\par \end{figure}$	Figure 14: Height-time plot for the lifting flux rope as seen by TRACE and LASCO C2 with error bars representing five pixels. The dashed line represents the continuation of the exponential fit to the TRACE data. This is followed by the velocity profile and acceleration profile derived from the first and second derivative of the fits to the data.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2321fi15.ps}\end{figure}$	Figure 15: Cartoon representing the entire event, based upon our observations from all instruments.
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