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\@writefile{toc}{\contentsline {section}{\numberline {A}Proposal Summary}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {B}Project Description}{1}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.1}Results from Prior ATM Support (April 2004 to June 2007)}{1}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.1}High Cadence Flare Observations}{1}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Above: RHESSI HXR light curve of 2002 September 9 fare, in the energy band of 25 to 50 keV for which the time resolution is 4 s. (b) Time profile of centroid distance between the two conjugate kernels, for which the cadence is 40 ms. (c) Time profile of centroid distance with error bars, which is rebinned according to the RHESSI HXR 4 s time resolution. The dotted lines indicate the rising periods of four HXR spikes (Ji et al., 2004b). }}{2}}
\newlabel{FIG01}{{1}{2}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.2}Rapid Evolution of Magnetic Fields Associated with Flares}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces TRACE WL images revealing the rapid change of $\delta $ sunspot structure associated with four major flares. The top, middle, and bottom rows show the pre-flare images, post-flare images, and the difference images between them, respectively. The white feature in the difference image indicates the region of penumbral decay, while the dark feature indicates the region of central umbral/penumbral enhancement (Adapted from Liu et al. 2005).}}{3}}
\newlabel{FIG02}{{2}{3}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.3}Relationship among Filament Eruptions, Flares, CMEs and Magnetic Reconnection}{4}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.4}Application of Artificial Intelligence in Detection and Characterization of Solar Activity}{4}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.1.5}Selected BBSO Publications from March 2004 to June 2007}{4}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.2}Current Instrumentation Projects}{5}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.1}New Solar Telescope}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces A recent diffraction-limited image obtained at BBSO on April 29, 2005 with the AO-76 system and speckle reconstruction.}}{6}}
\newlabel{FIG03}{{B.2.2}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.2}Adaptive Optics (AO)}{6}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.2.3}Imaging Magnetograph Systems}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces The sample result of recent IRIM observations with the adaptive optics system at BBSO. It includes the true-field strength $(a)$, magnetic flux $(b)$ and filling factor $(c)$ maps of NOAA Active Region 10781 (Cao et al., 2006). The bottom plot is the example of Stokes-V fitting using two NIR lines simultaneously.}}{7}}
\newlabel{FIG04}{{4}{7}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.3}Sub-arcsecond, Sub-second Structure of Flares}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces NIR time sequence of the X10 flare from 20:40\nobreakspace  {}UT to 20:47\nobreakspace  {}UT on 2003 October\nobreakspace  {}29. RHESSI HXR contours (blue) correspond to the $50$ - $100$\nobreakspace  {}keV channel with 60 integration. The local NIR intensity maxima are shown in red. Two flare ribbons are correlated with strong HXR kernels. HXR contour levels are drawn at 0.17, 0.25, 0.60, and 0.80 of the maximum intensity, except for the first two frames, where they correspond to 0.7 and 0.8 for the first frame and 0.4, 0.6, and 0.8 for the second, when the HXR kernels were weaker.}}{9}}
\newlabel{FIG05}{{5}{9}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.4}Quantitative and Systematic Studies of Evolution of Magnetic Fields Associated with Flares}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces Left, a vector magnetogram of September 13, 2005 observed at BBSO. Right: The time profile of the mean transverse field strength in 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{FIG06}{{6}{11}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.5}Surface Flows Associated with Flares and CMEs }{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Left: TRACE WL image at 0201\nobreakspace  {}UT before the onset of the X3.4 flare on 2006 December 13. Middle: WL image after the flare at 0508\nobreakspace  {}UT. Right: the difference between post- and preflare WL intensity. The enhancement of sunspot structure at the flaring neutral line and peripheral penumbral decay are quite obvious.}}{12}}
\newlabel{FIG07}{{7}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces High resolution vector magnetogram processed from Spectro-Polarimeter of SOT. The top images are preflare observation at 2030\nobreakspace  {}UT on December 12, while the bottom images are postflare observations at 0430\nobreakspace  {}UT on December 13. Left panels show G-band images, while right panels show transverse magnetic vectors overlying on longitudinal magnetograms.}}{13}}
\newlabel{FIG08}{{8}{13}}
\@writefile{toc}{\contentsline {subsection}{\numberline {B.6}High Resolution Near IR Observations Non-Flaring Solar Atmosphere}{13}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.6.1}Contribution of Footpoint Motion to Coronal Loop Heating}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces Photospheric flows and magnetic field configuration of NOAA\nobreakspace  {}10486 on 2003 October\nobreakspace  {}29. To illustrate the results of high spatial resolution local correlation tracking analysis of WL data observed by the BBSO team at NSO/SP, we provide different views of (a) flow vectors, (b) azimuthal angle of the velocity vectors, (c) magnitude of the velocity vectors, and (d) MDI magnetogram with superimposed magnetic neutral lines. $I/I_0$ in (a) is the normalized intensity relative to quiet photosphere (Yang et al. 2004). Strong shear flows are found along flaring neutral line, denoted by S1 through S4; while K1 through K3 mark flare kernels.}}{14}}
\newlabel{FIG09}{{9}{14}}
\@writefile{toc}{\contentsline {subsubsection}{\numberline {B.6.2}Quite Sun Magnetic Fields below Intranetwork Fields}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {C}Personnel and Management}{15}}
\@writefile{toc}{\contentsline {section}{\numberline {D}References Cited}{16}}
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