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\@writefile{toc}{\contentsline {section}{\numberline {1}INTRODUCTION}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {2}DATA SOURCES}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {3}OBSERVATIONAL FINDINGS}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {4}SUMMARY AND DISCUSSION}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces A time sequence of BBSO H$\alpha $\nobreakspace  {}$-$\nobreakspace  {}0.6\nobreakspace  {}\r A\ images covering the 2005 September 13 X1.5 flare. The field of view is 300\unhbox \voidb@x \hbox {$^{\prime \prime }$}\nobreakspace  {}$\times $\nobreakspace  {}260\unhbox \voidb@x \hbox {$^{\prime \prime }$}. F is the erupting filament at the boundary of the AR. A, B, C and D are four initial flaring footpoints. $1a$, $1b$ and $2$ are three moving ribbons. The black box marked a section of magnetic neutral line that will be discussed in Figure\nobreakspace  {}5. }}{8}}
\newlabel{F1}{{1}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces The position of front of the three moving flare ribbons as a function of time. The solid line is the light curve of microwave at 10\nobreakspace  {}GHz observed by OVSA. The bottom panel shows the filament heights. Diamonds are points based on BBSO H$\alpha $ observations, while the stars are based on TRACE 195\nobreakspace  {}\r A\ observations. Straight lines are fittings to derive speeds of motions. }}{9}}
\newlabel{F2}{{2}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces TRACE 195\nobreakspace  {}\r A\ images showing the brightening of a large loop (denoted by arrow) that is co-spatial with the filament (``F''), and their final eruption after $\sim $19:35\nobreakspace  {}UT. }}{10}}
\newlabel{F3}{{3}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Time line of the 2005 September 13 X1.5 event described on the lightcurve of GOES soft X-ray flux at the 1--8\nobreakspace  {}\r A\ channel, showing the starting time of H$\alpha $ brightening ($\sim $19:22\nobreakspace  {}UT), TRACE loop brightening interval ($\sim $19:24--19:35\nobreakspace  {}UT), the flare peak time in GOES ($\sim $19:27\nobreakspace  {}UT), and the time of filament and TRACE loop eruption ($\sim $19:35\nobreakspace  {}UT). See \S  \nobreakspace  {}3 for detailed discussion. }}{10}}
\newlabel{F4}{{4}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces The time profile of the mean transverse field strength for the area marked by the black box in Figure\nobreakspace  {}1. This is the section of the neutral line close to the initial flare core. The timing of the flare is indicated by the 10\nobreakspace  {}GHz OVSA microwave light curve. }}{11}}
\newlabel{F5}{{5}{11}}