All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{h4228f01.ps}\end{figure}$ Figure 1: The GOES light curves for the X1.2 flare of 23 April 1998. Its C2.0 precursor at about 05:32 UT is clearly seen. The upper curve shows the emission in the 1-8 Å band, the lower curve shows the emission in the 0.5-4 Å band. Time intervals shown by the hatched areas indicate times when Yohkoh data were unavailable because of satellite night-time.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f02.ps}\end{figure}$ Figure 2: The light curves of the C2.0 precursor obtained in four channels of the BCS, in the channel L of the HXT, and in two channels of the GOES are shown. The fluxes are in cts s^-1, cts s^-1 SC^-1, and W m^-2 $\times$ 10⁵ units, for the BCS, HXT, and GOES, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f03.ps}\end{figure}$ Figure 3: A sequence of SXT HN AlMg images illustrating the evolution of the X-ray ejection. The continuous curve represents the solar eastern limb. Solar north is up, east to the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4228f04.ps}\end{figure}$ Figure 4: The SXT(AlMg) light curves of individual features seen in Fig. 3. See text for explanation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4228f05.ps}\end{figure}$ Figure 5: A plot representing the expansion of the leading (stars) and the trailing edge (boxes) of the X-ray ejection. The least-squares fit to data and example values of velocity are also shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f06.ps}\end{figure}$ Figure 6: An example of Al12/AlMg temperature maps of the NOAA AR 8210 before and during the X-ray ejection. Lines of constant temperature are overplotted on the SXT FN AlMg images. See the caption of Fig. 3 for more details.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4228f07.ps}\end{figure}$ Figure 7: The Al12/AlMg temperature changes for the selected parts of the NOAA AR 8210 before and during the X-ray ejection. See text for explanation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f08.ps}\end{figure}$ Figure 8: The time evolution of individual energy rates estimated for the X-ray ejection. See text for explanation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f09.ps}\end{figure}$ Figure 9: Running-difference images of LASCO/C2 ( upper three panels) and LASCO/C3 ( lower three panels), which show the evolution of the halo CME on 23 April 1998. Time is indicated at the top of each panel. The white circle in each panel indicates the solar limb ( $1.0~R_{\hbox{$\odot$ }}$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f10.ps}\end{figure}$ Figure 10: Running-difference images of EIT $\lambda$ 195 Å ( upper three panels) and LASCO/C1 $\lambda$ 5303 Å ( lower three panels), which show the early evolution of the halo CME on 23 April 1998. Time is indicated at the top of each panel. The white circle in each panel indicates the solar limb ( $1.0~R_{\hbox{$\odot$ }}$ ).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{h4228f11.ps}\end{figure}$ Figure 11: Height-time plot (dashed line) of the CME front on 23 April 1998. The CME heights were measured in LASCO images. Different symbols: asterisks, triangles, and squares denote C1, C2, and C3 images, respectively. The parabolas represent the position of the leading and the trailing edge of the X-ray ejection observed (Fig. 5) and extrapolated under assumption of their constant acceleration 0.95 km s^-2, and 0.44 km s^-2, respectively. Three straight lines coming out from the point at 05:55 UT represent an extrapolated position of the CME front under assumption of the constant velocity 540, 580, and 620 km s^-1, respectively. The estimated height of the X-ray ejection front from type II radio bursts is marked with crosses. The suggested place of the collision between the fronts of the CME and the X-ray ejection is marked by the arrow and additionally blown-up in the insert (upper left corner).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f12.ps}\end{figure}$ Figure 12: Velocity-time profile of the CME front on 23 April 1998. Two phases of impulsive acceleration are seen: the first somewhere between 04:51-05:27 UT, the second somewhere between 05:55-06:44 UT.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{h4228f01.ps}\end{figure}$	Figure 1: The GOES light curves for the X1.2 flare of 23 April 1998. Its C2.0 precursor at about 05:32 UT is clearly seen. The upper curve shows the emission in the 1-8 Å band, the lower curve shows the emission in the 0.5-4 Å band. Time intervals shown by the hatched areas indicate times when Yohkoh data were unavailable because of satellite night-time.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f02.ps}\end{figure}$	Figure 2: The light curves of the C2.0 precursor obtained in four channels of the BCS, in the channel L of the HXT, and in two channels of the GOES are shown. The fluxes are in cts s^-1, cts s^-1 SC^-1, and W m^-2 $\times$ 10⁵ units, for the BCS, HXT, and GOES, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f03.ps}\end{figure}$	Figure 3: A sequence of SXT HN AlMg images illustrating the evolution of the X-ray ejection. The continuous curve represents the solar eastern limb. Solar north is up, east to the left.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4228f04.ps}\end{figure}$	Figure 4: The SXT(AlMg) light curves of individual features seen in Fig. 3. See text for explanation.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4228f05.ps}\end{figure}$	Figure 5: A plot representing the expansion of the leading (stars) and the trailing edge (boxes) of the X-ray ejection. The least-squares fit to data and example values of velocity are also shown.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f06.ps}\end{figure}$	Figure 6: An example of Al12/AlMg temperature maps of the NOAA AR 8210 before and during the X-ray ejection. Lines of constant temperature are overplotted on the SXT FN AlMg images. See the caption of Fig. 3 for more details.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{h4228f07.ps}\end{figure}$	Figure 7: The Al12/AlMg temperature changes for the selected parts of the NOAA AR 8210 before and during the X-ray ejection. See text for explanation.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f08.ps}\end{figure}$	Figure 8: The time evolution of individual energy rates estimated for the X-ray ejection. See text for explanation.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f09.ps}\end{figure}$	Figure 9: Running-difference images of LASCO/C2 ( upper three panels) and LASCO/C3 ( lower three panels), which show the evolution of the halo CME on 23 April 1998. Time is indicated at the top of each panel. The white circle in each panel indicates the solar limb ( $1.0~R_{\hbox{$\odot$ }}$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=18cm,clip]{h4228f10.ps}\end{figure}$	Figure 10: Running-difference images of EIT $\lambda$ 195 Å ( upper three panels) and LASCO/C1 $\lambda$ 5303 Å ( lower three panels), which show the early evolution of the halo CME on 23 April 1998. Time is indicated at the top of each panel. The white circle in each panel indicates the solar limb ( $1.0~R_{\hbox{$\odot$ }}$ ).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{h4228f12.ps}\end{figure}$	Figure 12: Velocity-time profile of the CME front on 23 April 1998. Two phases of impulsive acceleration are seen: the first somewhere between 04:51-05:27 UT, the second somewhere between 05:55-06:44 UT.
Open with DEXTER