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\@writefile{toc}{\contentsline {section}{\numberline {A.}Results from Prior SRT Support}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.1}High Cadence Flare Studies}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.2}Study of Microflares}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.3}Magnetic Field Evolution and Flares}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.4}Study of Coronal Mass Ejections}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.5}Space Weather Forecasting}{3}}
\@writefile{toc}{\contentsline {subsection}{\numberline {A.6}Publications Under Current SRT Support}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Left panel: The median value of the $r_0$ (Fried parameter, a rough measure of the diffraction limit, $r_0\ge $ 5.5 cm is required for correction by AO) measurements from the S-DIMM instrument (principal site survey instrument, see www.atst.nso.edu/site/ for details) at the three sites (Big Bear, \special {color push Red}Haleakala\special {color pop}, and \special {color push Blue}La Palma\special {color pop} as a function of hour angle (adapted from Figure\nobreakspace  {}10.13 in Hill et al.\ 2004). Right panel, BBSO often obtains diffraction limited images, even without AO system. This is an example of such a high resolution image in green continuum.}}{5}}
\newlabel{FIG01}{{1}{5}}
\@writefile{toc}{\contentsline {section}{\numberline {B.}Proposed Research}{5}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.1}Current Instrumentation Projects}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.1}New Solar Telescope (NST) at BBSO}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.2}Adaptive Optics}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.3}Visible Light Vector Magnetographs}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.4}Infrared Vector Magnetograph}{7}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.5}Real-Time Speckle Phase-Diversity Imaging}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces BBSO vector magnetogram obtained on October 19, 2001. The background is a BBSO H$\alpha $ image during an X1.6 flare. Green arrows indicate the transverse fields, red and blue contours are for negative and positive line-of-sight magnetic field strength, respectively. The thick, solid black lines are the neutral lines of the line-of-sight magnetic field.}}{8}}
\newlabel{FIG02}{{2}{8}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.2}Scientific Programs}{8}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.1}Evolution of Vector Magnetic Fields Associated with Solar Flares}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Comparison of pre-flare (a, e) and post-flare (b, f) states for the X10 flare on 2003 October 29. (a, b) and (e, f) are TRACE WL and 195\nobreakspace  {}\r A\ images, respectively. (c) is the WL difference image (the post-flare image minus the pre-flare image). (d) is the WL image at flare maximum with superimposed \textit  RHESSI 50-100 keV hard X-ray contours. D1 and D2 are two areas of penumbral decay and E is the center enhanced sunspot region (Liu et al., 2005).}}{9}}
\newlabel{FIG03}{{3}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Left panel: mean intensity of the penumbral decay areas D1 and D2 and the central darkening area E, of the previous figure, as a function of time on 2003 October 29 and the evolution of the absolute value of the longitudinal magnetic flux in each area. The curve of vertical spikes represents the RHESSI hard X-ray counts in the 50-100 keV range. Right Panel: A schematic interpretation of our observations. (a) Initial magnetic field configuration before the flare. Penumbral fields are in \textit  {grey} and umbral fields are in \textit  {black}. (b) Magnetic field configuration in the post-flare state. The dash-dot line in (b) represents the connection between two footpoints far apart, which may form the large-scale arcade structure of the CME. Note that the footpoint separation should be much larger than shown in the drawing (Liu et al., 2005).}}{10}}
\newlabel{FIG04}{{4}{10}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.2}Synoptic Observations and Space Weather Forecasting}{10}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.3}High Cadence Flare Observations}{12}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.4}High Resolution Visible and Near IR Observations of Active Regions}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Photospheric flows and magnetic field configuration of NOAA\nobreakspace  {}10486 on 2003 November\nobreakspace  {}29. To illustrate the high-spatial resolution results of local correlation tracking analysis of WL data observed by BBSO team at NSO/SP, we provide different views of (a) flow vectors, (b) azimuth angle of the velocity vectors, (c) magnitude of the velocity vectors, and (d) MDI magnetogram with superimposed magnetic neutral lines (Yang et al., 2004). $I/I_0$ in (a) in normalized intensity relative to quiet photosphere}}{14}}
\newlabel{FIG05}{{5}{14}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.3}Personnel}{15}}