\relax 
\@writefile{toc}{\contentsline {section}{\numberline {A}Proposal Summary}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {B}Introduction and Objectives of Proposed Research}{1}}
\@writefile{toc}{\contentsline {section}{\numberline {C}Research Plan}{2}}
\@writefile{toc}{\contentsline {subsection}{\numberline {C.1}Relationship Between Filament Disappearances and CMEs}{2}}
\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces Distribution of filament disappearance as function of the distance from the disk center. The lighter histogram is the total number of events, and the darker histogram is the number of events with associated CMEs found from the LASCO data. We also indicated at the top of each bar the percentage of events for which LASCO events have been identified.}}{3}}
\newlabel{FIG01}{{C.1}{3}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces The sequence of H$\alpha $ full-disk images demonstrating the disappearance of a major filament inside the white box. A Kitt Peak magnetogram at 15:43 on October 13 is also included to show the magnetic configuration. In the second row, we show a magnified field of view from the same images in the first row to demonstrate that the fine structure can be resolved by our full disk images.}}{4}}
\newlabel{FIG02}{{C.1}{4}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces Comparison of a CME observed on December 9, 2006 as observed by COR2/SECCHI on board STEREO (left) and a full disk Halpha obtained at BBSO on December 11, 2006. This simulates the situation when the STEREO has a view angle of about 24 degrees away from earth's observations. Then the center region active region's CME will be view clearly as limb event. }}{5}}
\newlabel{FIG03}{{3}{5}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Left panel: time profiles of the flare ribbon separation, filament heights measured from KSO and EIT images, and CME heights measured by Dr. Yashiro ($http://cdaw.gsfc.nasa.gov/CME\_list/$). The lines indicate the least-squares fits to hyperbolic functions. Right: velocity profiles of the ribbon separation, filament, and CME derived from the fits of the height profiles. }}{6}}
\newlabel{F4}{{4}{6}}
\@writefile{toc}{\contentsline {subsection}{\numberline {C.2}Helicity Injection Associated with Filament Eruptions}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces Time profiles of helicity injection, magnetic flux and GOES X-ray flux for 4 active regions. The helicity is shown as crosses; the dotted lines are the GOES X-ray flux and total average magnetic flux are shown as diamonds. The flux is averaged of the absolute sum of positive and negative fluxes. }}{8}}
\newlabel{F5}{{5}{8}}
\@writefile{toc}{\contentsline {subsection}{\numberline {C.3}The Relationship between the Rate of Magnetic Reconnection and Solar Eruptions}{9}}
\newlabel{eq1}{{5}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces Top panels: snapshot of an M1.0 flare in H$\alpha $ observed by KSO on 2000 September 12 and corresponding MDI magnetogram. Plus signs are trajectories of the ribbon fronts; colors from purple to white indicates a 2 hr time lapse from 11:00 to 13:00 UT. Bottom panels: Left: magnetic reconnection rate in terms of $E_c$ (red) and $\varphi _c$ (blue) in comparison with the time derivative of the GOES soft X-ray emission (dark) for the M1.0 event on 2000 September 12. Right: magnetic reconnection rate in terms of $E_c$ (red) and $\varphi _c$ (blue) in comparison with the microwave light curve at 6.6\nobreakspace  {}GHz (dark) for the X1.6 event on 2001 October 19 (Qiu et al., 2004).}}{10}}
\newlabel{FIG06}{{6}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces Top-left: Scatter plot of maximum filament acceleration vs. maximum $\varphi _{rec}$; Bottom-left: Scatter plot of maximum filament acceleration vs. maximum $E_{rec}$. Top-right: Scatter plot of CME velocity at C2 vs. maximum $\varphi _{rec}$; Bottom-right: Scatter plot of CME velocity vs. maximum $E_{rec}$. Error bars attached to each sign indicate the uncertainty of the measurement (Jing et al., 2005). }}{11}}
\newlabel{FIG05}{{C.3}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces Scatter plot of CME velocities vs. total reconnection flux for 13 events. Dark and gray colors indicate events associated with erupting and non-erupting filaments, respectively. The dashed guideline shows the least-squares linear fit to the data points (Qiu and Yurchyshyn, 2005).}}{12}}
\newlabel{FIG06}{{8}{12}}
\@writefile{toc}{\contentsline {section}{\numberline {D}Personnel and Budget}{13}}
\@writefile{toc}{\contentsline {section}{\numberline {E}References Cited}{14}}