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\@writefile{toc}{\contentsline {section}{\numberline {A.}Results from Prior ATM Support}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.1}High Cadence Flare Studies}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.2}Evolution of Magnetic Field During Flares}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.3}Study of CMEs}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.4}Space Weather Forecasting}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.5}Publications Supported by the Current ATM Support}{3}}
\@writefile{toc}{\contentsline {section}{\numberline {B.}Proposed Research}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.1}On Going Instrumentation Projects}{5}}
\@writefile{toc}{\contentsline {subsubsection}{Adaptive Optics}{5}}
\@writefile{toc}{\contentsline {subsubsection}{New Telescope at BBSO}{5}}
\@writefile{toc}{\contentsline {subsubsection}{Visible Light Vector Magnetographs}{6}}
\@writefile{toc}{\contentsline {subsubsection}{Infrared Vector Magnetograph}{6}}
\@writefile{toc}{\contentsline {subsubsection}{Global H$\alpha $ Network}{7}}
\@writefile{toc}{\contentsline {subsubsection}{Real-Time Speckle Imaging}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces A DVMG vector magnetogram from October 19, 2001. The background is an H$\alpha $ image during an X1.6 flare. Arrows indicate the transverse fields, and the thick, solid black lines are the neutral lines of the line-of-sight magnetic field.}}{8}}
\newlabel{fig:vector}{{1}{8}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.2}Scientific Programs}{8}}
\@writefile{toc}{\contentsline {subsubsection}{Evolution of Vector Magnetic Fields Associated with Solar Flares}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces Magnetic flux, mean transverse magnetic field and weighted mean magnetic shear as a function of time for July 26, 2002 event, overplotted by GOES X-ray flux.}}{9}}
\newlabel{fig:020726a}{{2}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Line-of-sight magnetogram, H$\alpha $ and RHESSI (blue contours) flare emission, and transverse fields before and after the flare. The red circle marks the area where transverse field and magnetic shear had an sudden increase associated with the flare.}}{9}}
\newlabel{fig:020726b}{{3}{9}}
\@writefile{toc}{\contentsline {subsubsection}{Synoptic Observations and Space Weather Forecasting}{9}}
\@writefile{toc}{\contentsline {subsubsection}{Helicity Injection into Erupting Filaments, CMEs and Flares}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Temporal change of magnetic helicity change rate (thick solid line), GOES X-ray intensity (dotted line), and the sum of the norms of the photospheric velocity vectors (thin solid line) expressed in an arbitrary scale for the November 24, 2000 flares.}}{12}}
\newlabel{fig:moon}{{4}{12}}
\@writefile{toc}{\contentsline {subsubsection}{High Cadence Flare Observations}{12}}
\@writefile{toc}{\contentsline {subsubsection}{High Resolution Visible and Near IR Observations of Active Regions}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Left panel: a line-of-sight DVMG image of November 24, 2000. The white rectangle marks a magnetic channel structure. The field-of-view is 150$\times $180 arcsec. Right panel: H$\alpha $ image of the X2 flare at 21:53UT, in the same field of view as the magnetogram. An erupting flux rope is denoted by $``$F'', and the black contours show Yohkoh hard X-ray kernels.}}{14}}
\newlabel{fig:channel}{{5}{14}}