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HR.aux
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\@writefile{lof}{\contentsline {figure}{\numberline {4.1}{\ignorespaces Mosaic of speckle reconstructed broadband images of the active region NOAA AR0621, at $\mu $\,=\,0.68. The achieved high resolution by means of the adaptive optics and {\em post factum} reconstruction is $\sim 0.2\hbox {$^{\prime \prime }$}$. The total area covered is $\sim $\,103\hbox {$^{\prime \prime }$}$\times $94\hbox {$^{\prime \prime }$}. Limb is located to the left lower corner.}}{47}{figure.4.1}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.2}{\ignorespaces H$\alpha $ line center filtergram. It corresponds to one of the 18 reconstructed images along the spectral line. The resolution in these narrow-band images is $<$\,0.5\hbox {$^{\prime \prime }$}. One notes the various chromospheric features: ubiquitous short fibrils with different orientation, a wide bright plage region full of facular grains on the lower central part, and dark fibrils packed together outlining the magnetic field lines between sunspots around the central data gap. White arrow indicates position and direction of the dark cloud in Fig. \ref {fig:cloud}}}{47}{figure.4.2}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.3}{\ignorespaces \emph {Left}: Motion of dark feature seen in H$\alpha $ at +1 \r A\,off line center, presented in false color to increase contrast. Vertical red lines are separated by 3.15\hbox {$^{\prime \prime }$}($\sim $\,2280 km). Time step between consecutive images $\sim $\,45 s. Horizontal tiles represent consecutive frames from the time sequence (from top to bottom). \emph {Right}: Spectral profiles, normalized to the quiet Sun spectrum at 6562 \r A, of the central part of one of the cloud members, marked by white crosses on the left image. Black solid line is the mean profile of the surrounding quiet Sun.}}{48}{figure.4.3}}
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\@writefile{lot}{\contentsline {table}{\numberline {4.1}{\ignorespaces Several derived parameters from the cloud model for the lower half section of the long fibril in Fig.\nobreakspace {}\ref {fig3} at $t=25$ min. We assume a LOS thickness equal to the width of the fibril ({cylindrical} shape) of $590$ km and a micro-turbulent velocity of $10$ km/s. First two rows result from the inversion technique while the others are parameters derived from them.}}{54}{table.4.1}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.8}{\ignorespaces Simultaneous flash event on AOIs B and B\hbox {$^\prime $}\ with projected distance $\approx $13.7 Mm. A pair of simultaneous, short, brightening was recorded at $t=52.2$ min. Top row from B\hbox {$^\prime $}, bottom row from B. The tiles from left to right correspond to two successive H$\alpha $ scans. Upper x-axis is scaled to the wavelength of each 2-D filtergram tiles. Scanning time is numbered on the lower x-axis. $t=0$ corresponds to the beginning of the scan at 08:44 UT. The integration time for each spectral position is $\approx 1$s, while the delay between two scans is $\approx 3$s (vertical dashed line). Each spectrogram on B is normalized with the background profile (see Fig. \ref {fig5}) to emphasize the flash event. Neither the previous nor the following scan to the two presented exhibited any emission. The second scan (right half size of the figure) still shows some emission on the same positions. White arrows correspond to the position of the three different profiles in Fig. \ref {fig5}.}}{58}{figure.4.8}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.9}{\ignorespaces H$\alpha $ profiles from the flash event. Each profile corresponds to an average over three pixels around the three selected points where the emission is highest in the blue wing, at central wavelength, and in the red wing respectively, corresponding to the white arrows in Fig. \ref {fig4} (left half) at x=[3.7, 2.8, 1.1]\nobreakspace {}Mm, respectively. For comparison the quiet Sun profile is also shown. Background profile corresponds to the mean from previous and following scans, where no brightening was found. The emission profile at 1.1\nobreakspace {}Mm reaches an intensity of 1.1 of the quiet Sun continuum intensity.}}{59}{figure.4.9}}
\newlabel{fig5}{{4.9}{59}{Synchronous flashes\label {mini-flare}\relax }{figure.4.9}{}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.11}{\ignorespaces Example of space-time slices, of 1\hbox {$.\mskip -\thinmuskip \mskip -\thinmuskip ^{\prime \prime }$}1 width, from AOI C in Figs.\nobreakspace {}\ref {fig1} and \ref {fig2}. From left to right: LOS velocity, H$\alpha $ line center intensity, and intensity differences at H$\alpha $\nobreakspace {}+0.5\r A\ off line center: $I_{0.5}(t_{i+1})-I_{0.5}(t_{i})$ with cadence of $\Delta t=t_{i+1}-t_{i}$\,= 22\nobreakspace {}s. The intensity differences in the right column are shifted up by 11\nobreakspace {}s. They are referred to as $\Delta I_{0.5}$ slices in the text.}}{65}{figure.4.11}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.15}{\ignorespaces Results for different image reconstruction techniques. Axes are in arcseconds. White rectangles enclose the region where the RMS contrast is calculated. \emph {Upper left}: Best speckle raw image, contrast is 5.9\%. \emph {Upper right}: SI+AO result, contrast is 11.1\%. \emph {Lower left}: MOMFBD running 17 modes, contrast is 6.7\%. \emph {Lower right}: MOMFBD running 100 modes, contrast is 10.0\%.}}{75}{figure.4.15}}
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\@writefile{lof}{\contentsline {figure}{\numberline {4.17}{\ignorespaces Results for different image reconstruction techniques for the line center narrow-band filtergram. Scales on the axes are in arcseconds. \emph {Upper left}: Best speckle raw image.\,\emph {Upper right}: SI+AO result. \emph {Lower left}: MOMFBD running 17 modes. \,\emph {Lower right}: Image difference. In this case the differences reach 45\% of the fluctuations in the reconstructed frames.}}{76}{figure.4.17}}
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