All Figures

$\begin{figure} \par\hbox{\hspace*{0.3cm} \resizebox{8.20cm}{!} {\includegraphics... ... {\includegraphics[width=8.20cm,height=4.825cm]{0660fg1f.eps} }% }\end{figure}$ Figure 1: Temporal and spatial behaviour ( $\rm 2.5~min\times6.3''$ ) of the Fe II 6456.38 Å spectral line characteristics $I_{\rm c}$ , $I_{\rm r}$ , $v_{\rm d}$ , $f_{\rm w}$ , and $e_{\rm w}$ around the selected $f_{\rm w}$ -event (position 3.3''). No correction for the 5 min velocity oscillations was performed leaving the zero level of $v_{\rm d}$ uncertain to within several hundreds of m/s. The limb is in the downward direction of the plots. The spatial scale of the plots should be multiplied by a factor of 1.538 to obtain real distances on the solar surface. The actual seeing conditions traced from the temporal variations of the $I_{\rm c}$ rms-contrast are shown in the bottom right panel. The vertical structure in the plots is caused by different seeing quality. The image jitter at the entrance slits, caused by seeing, does not lead to a reduction of contrast of the spectral characteristics (e.g. around the time 0.5 min). Occasional low spatial gradients of observed spectral characteristics are due to moments of bad observational conditions (e.g. as around 0.8 and 1.5 min).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=18cm,height=18.1cm]{0660fig2.eps} \end{figure}$ Figure 2: Representative spatial scans of the Fe II 6456.38 Å spectral characteristics for three time instances (0.05, 0.4 and 1.16 min) during the event (solid lines of different thickness) and for a reference time (dashed line). The scans were extracted from Fig. 1. The temporal evolution of the line width, $f_{\rm w}$ , of the considered $f_{\rm w}$ -event is shown in the bottom right panel where the selected time instances are indicated by vertical lines of the corresponding line thickness used in the other panels. The solar limb is in the downward direction in all the plots. The spatial scale must be multiplied by a factor of 1.538 to get real distances on the solar surface. Dotted lines show the average values of the characteristics over a slit length of 80'' and over a time of 15 min.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=9.0cm,width=8.8cm]{0660fig3.eps} \par\end{figure}$ Figure 3: Profiles of the Co I 6455.0 Å, Ca I 6455.6 Å, and Fe II 6456.38 Å spectral lines of the $f_{\rm w}$ -event. Upper panel: the line profiles taken during the $f_{\rm w}$ -event (t=0.05 min at slit position 3.3'') drawn with solid line together with the corresponding reference spectrum (dashed). The reference spectrum was prepared from spectra taken at the same centre-to-limb distance averaging several exposures around the time t=2.5 min. The relative difference of the spectra calculated with an identical continuum intensity is shown in the bottom panel. The vertical dashed lines mark the line centre positions of the reference spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\hbox{\hspace*{1.1cm} \resizebox{7.7cm}{!} {\includegraphics[... ...{!} {\includegraphics[height=7.0cm,width=7.0cm]{0660fg4d.eps}} % }\end{figure}$ Figure 4: Evolution of the G-band SJ image in the surroundings of the $f_{\rm w}$ -event. The four panels show the temporal changes from the upper left to the bottom right panel with the time information given in their titles. The first three images trace the G-band bright point just near the edge of the slit. The last image shows the field after the $f_{\rm w}$ -event has diminished. The position of the slit is marked by the vertical dark rectangle. The $f_{\rm w}$ -event is centred in the middle of the images at 3.3''. The solar limb is directed toward the bottom of the images.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6.0cm,width=8.8cm]{0660fig5.eps} \end{figure}$ Figure 5: Temporal evolution of the maximum intensity of the G-band bright point. The figure shows the maximum intensity of the bright point (solid line), the maximum intensity of the granular pattern found on the opposite side of the slit (dotted line), and the average intensity of the G-band image (dashed line). The triangles mark the first three G-band images shown in Fig. 4.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=8.8cm,width=8.0cm]{0660fig6.eps} \end{figure}$ Figure 6: Spectral signature of a discontinuous flow field with v_x(x) = v₀ for x<0 and v_x(x) = 0 for $x \ge 0$ embedded in a plane parallel standard solar atmosphere. The spectral line of Fe II 6456.38 Å is computed along slanted lines-of-sight ( $\cos\theta = 0.643$ ) and corresponding Doppler-shifts ( bottom) and FWHM ( top) are plotted as a function of the spatial position of the ray entry-point at a height of 800 km above $\tau _{\rm c} = 1$ . The solid curves are obtained with the full spatial resolution of 10 km, the dashed curve when applying a Gaussian blur of 0.25''width using neighbouring ray profiles, and the dotted curves when applying an additional box-car average of 0.5'' width mimicking a shock front that is inclined by $45^{\circ }$ with respect to the spectrograph slit.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.0cm,width=8.6cm]{0660fig7.eps} \end{figure}$ Figure 7: Histogram of the normalized line widths, $f_{\rm w,~N}$ (thick solid histogram). The central component of this distribution is fitted by a Gaussian profile (dashed line). The secondary component, representing excess values of $f_{\rm w,~N}$ (cross-hatched region) was determined as the difference between the positive ( right) and the negative ( left) part of the distribution. Its fractional area is 0.45% of the total area of the distribution. The dotted vertical line marks the position of the Gaussian fit for the central component. The histogram includes a total of $18\times 10^{4}$ values of $f_{\rm w,~N}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=6.0cm,width=8.8cm]{0660fig5.eps} \end{figure}$	Figure 5: Temporal evolution of the maximum intensity of the G-band bright point. The figure shows the maximum intensity of the bright point (solid line), the maximum intensity of the granular pattern found on the opposite side of the slit (dotted line), and the average intensity of the G-band image (dashed line). The triangles mark the first three G-band images shown in Fig. 4.
Open with DEXTER