All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{1380fig1.eps} \end{figure}$ Figure 1: Subfield of one of our best G-band ( left) and blue continuum ( right) filtergrams. The arrow marks the direction to disk center. The full field of view amounts to $87\times70~{\rm arcsec}^{2}$ . The images are corrected for atmospheric distortions using the speckle masking method, and reach the theoretical resolution limit of the telescope of 0.2 arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1380fig2.eps} \end{figure}$ Figure 2: Examples of dark-cored filaments observed in the center-side penumbra. Each of the columns shows ( from top to bottom) G-band intensity, continuum intensity, and a bottom-to-top cut through the structure at the position indicated in the images. Distances are expressed in arcsec. The intensities are normalized to the mean quiet sun intensity. Each image is rotated to similar orientation. Solid: G band. Dashed: blue continuum. The dotted profile in the first plot depicts the Airy point-spread function of the telescope at 430.5 nm, with a FWHM of 0.2 arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1380fig3.eps} \par\end{figure}$ Figure 3: Temporal evolution of a dark-cored filament between 10:21 a) and 11:36 UT h). For better visibility a non-linear intensity scale ( $\gamma =1.6$ ) is used. Tick marks are arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1380fig4.eps} \end{figure}$ Figure 4: Top: Sketch of isotherms in a sunspot observed at an heliocentric angle of 27 deg. The arrows indicate lines of sight intersecting the center and limb-side penumbra. The dotted lines represent the normal to the isotherms. Bottom: Cross section of the same penumbral flux tube observed in the limb-side ( left) and center-side ( right) penumbra. The shaded areas in the tube interior represent plasma at lower temperature. The dotted lines mark isolines of optical depth. Depicted are three rays piercing the central and lateral parts of the tube. In the center-side penumbra, $\tau = 1$ is reached in the top part of the tube along the central ray, and in the hotter interior along the lateral rays. This would be observed as two bright streaks separated by a central obscuration.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1380fig5.eps} \end{figure}$ Figure 5: Subfield of a G-band filtergram of NOAA 10008 taken on June 28, 2002. The arrow depicts the direction towards disk center. The heliocentric angle of the spot is 48 deg ( $\mu =0.67$ ). Consistent with our findings, dark-cored filaments are observed predominantly in the center-side penumbra.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{1380fig1.eps} \end{figure}$	Figure 1: Subfield of one of our best G-band ( left) and blue continuum ( right) filtergrams. The arrow marks the direction to disk center. The full field of view amounts to $87\times70~{\rm arcsec}^{2}$ . The images are corrected for atmospheric distortions using the speckle masking method, and reach the theoretical resolution limit of the telescope of 0.2 arcsec.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1380fig3.eps} \par\end{figure}$	Figure 3: Temporal evolution of a dark-cored filament between 10:21 a) and 11:36 UT h). For better visibility a non-linear intensity scale ( $\gamma =1.6$ ) is used. Tick marks are arcsec.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1380fig5.eps} \end{figure}$	Figure 5: Subfield of a G-band filtergram of NOAA 10008 taken on June 28, 2002. The arrow depicts the direction towards disk center. The heliocentric angle of the spot is 48 deg ( $\mu =0.67$ ). Consistent with our findings, dark-cored filaments are observed predominantly in the center-side penumbra.
Open with DEXTER