\relax 
\@writefile{toc}{\contentsline {section}{\numberline {1.}INTRODUCTION}{1}}
\@writefile{lot}{\contentsline {table}{\numberline {1}{\ignorespaces The characteristics of investigated flares. }}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2.}DATA ANALYSIS}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces \em  X-ray emission contours for soft (solid line) and hard (dotted) X-ray ranges drawn atop the optical images (grey scale) for eight flares analysed. }}{2}}
\newlabel{fig:fig1}{{1}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces \em  Light curves for the 10$^{\fam 0 \ninerm th}$ November 1991 flare as measured by GOES (0.5 - 4 \r A) and HXT (M2 channel 33 - 53 keV). Dotted vertical lines correspond to times of the images presented in the next Figure. }}{2}}
\newlabel{fig:fig2a}{{2}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces \em  The time sequence of 6 images for the 10$^{\fam 0 \ninerm th}$ November 1991 flare. The optical image is presented in the grey scale while soft (SXT Al12 ) and hard (HXT M2 channel) emissions are shown as solid and dashed contours respectively.}}{2}}
\newlabel{fig:fig2}{{3}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces \em  Light curves for the 13$^{\fam 0 \ninerm th}$ November 1991 flare as measured by GOES (0.5 - 4 \r A) and HXT (M2 channel 33 - 53 keV). Dotted vertical lines correspond to times of the images presented in the next Figure.}}{3}}
\newlabel{fig:fig3a}{{4}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces \em  Time sequence of four images for 13$^{\fam 0 \ninerm th}$ November 1991 flare. The optical image is presented in the grey scale while soft (SXT Al12 data) and hard (M2 HXT channel) X-ray emissions are shown as solid and dashed contours respectively.}}{3}}
\newlabel{fig:fig3}{{5}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces \em  Light curves for the 15$^{\fam 0 \ninerm th}$ November 1991 flare as measured by GOES (0.5 - 4 \r A) and HXT (M2 channel 33 - 53 keV). Dotted vertical lines correspond to times of the images presented in the next Figure.}}{4}}
\newlabel{fig:fig6a}{{6}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces \em  The time sequence of the six images for the 15$^{\fam 0 \ninerm th}$ November 1991 flare. The optical image is displayed using the grey scale while soft (SXT Al12) and hard (HXT M2 channel) emissions are shown as solid and dashed contours respectively.}}{4}}
\newlabel{fig:fig6}{{7}{4}}
\@writefile{toc}{\contentsline {section}{\numberline {3.}SUMMARY AND CONCLUSIONS}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces \em  The evolution of maximum brightness location presented as coloured contours drawn at 0.8 of maximum intensity for Al12 deconvolved images. The contours are overlied atop the emission pattern (in grey) of the first unsaturated SXT Al12 image within the sequence.}}{5}}
\newlabel{fig:fig4}{{8}{5}}
\bibcite{Har92}{\astroncite {Hara}{1992}}
\bibcite{Moon99}{\astroncite {Moon}{1999}}
\bibcite{Sak92}{\astroncite {Sakao}{1992}}
\bibcite{Syl98}{\astroncite {Sylw98}{1998}}
\bibcite{Syl99}{\astroncite {Sylw99}{1999}}