Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f1.ps} \end{figure}$ Figure 1: Maps of the disk centre sunspot from Sep. 23, 2003, showing spectrally integrated Stokes-I, -Q, -U, and -V absolute values.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{2042f2.ps} \end{figure}$ Figure 2: Response of Stokes I ( left panels) and V ( right panels) to temperature ( upper panels), velocity ( middle panels) and magnetic field ( lower panels) for Fe I 10783 Å ( left columns), Si I 10784.5 Å ( middle columns), and Si I 10786.8 Å ( right columns) for a quiet Sun atmosphere ( upper rows), mean penumbral atmosphere ( middle rows) and hot umbral atmosphere ( lower rows); each subpanel spans ordinates from $\log\tau$ = 1.2 to $\log\tau$ = -4 and abscissa of 2 Å.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip] {2042f3.ps} \end{figure}$ Figure 3: Response functions (RF) of Stokes-I to temperature in a quiet sun atmosphere ( left panels), to LOS velocity in a penumbral atmosphere ( middle panels) and of Stokes-V to magnetic field in a hot umbral atmosphere ( right panels) at different positions throughout the three lines observed.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2042f5.ps} \end{figure}$ Figure 4: Circular paths selected to determine azimuthal means of the deduced parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f6.ps} \end{figure}$ Figure 5: Temperature as a function of $\log\tau_{5000}$ for umbra ( left) and mean penumbra ( right panel). Solid lines: darkest umbral core with SIR-adapted straylight; dotted lines: with a constant straylight of 5%; long-dashes: Mathew et al. (2003); short dashes ( left panel): cold umbral model by Stellmacher & Wiehr (1981); dot-dashes ( left panel: cold umbral model by Collados et al. (1994); three-dot-dashes ( left panel): hot umbral model by Collados et al. (1994); three-dot-dashes ( right panel): mean penumbral model by del Toro Iniesta et al. (1994).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f7.ps} \end{figure}$ Figure 6: Radial variation of azimuthally averaged intensity ( left panel) in the continuum ( upper curve), the line core ( lower curve) and line positions in between, together with temperatures ( middle panel) for $\log\tau$ = 0 ( upper curve), $\log\tau$ = -0.5 ( upper middle curve), $\log\tau$ = -1 ( lower middle curve), $\log\tau$ = -2 ( lower curve), and micro-turbulence ( right panel), as a function of the radial distance from the sunspot centre. Deduced quantities assuming a constant straylight factor of 5% or free SIR-adopted straylight are denoted by solid lines and dashed lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f8.ps} \end{figure}$ Figure 7: Velocity maps of the disk centre spot at different layers; negative values denote upflows; the contours mark the outer boundary of umbra and penumbra.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f8b.ps} \end{figure}$ Figure 8: Radial variation of azimuthally-averaged LOS velocities retrieved with 5% constant straylight (solid-thick line) and SIR-adapted straylight (dashed-thin line) for different heights. Error bars represent the velocity standard deviations in each radial bin and triangles their extreme values.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,bb=22 3 497 269,clip]{2042... ....ps}\hspace{2mm} \includegraphics[width=8.3cm,clip]{2042f10d.ps} }\end{figure}$ Figure 9: Maps of the vertical ( upper) and the horizontal ( second) components of the magnetic field vector, its inclination ( third) and its azimuth ( lower panel) at 4 different atmospheric height levels marked in each sub-panel. The contours mark the outer boundary of the umbra and of the penumbra.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f11.ps} \end{figure}$ Figure 10: Scatter-plots of strength and inclination of the magnetic field for the height levels $\log\tau$ = 0 ( upper left), $\log\tau$ = -0.5 ( upper right), $\log\tau$ = -1.0 ( lower left), and $\log\tau$ = - 2 ( lower right).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip] {2042f9.ps} \end{figure}$ Figure 11: Radial variations of the azimuthally-averaged field azimuth, field strength and field inclination; the latter two are presented for 5% constant straylight and for SIR-adapted straylight. Each sub-figure contains 4 height levels.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip] {2042f12.ps} \end{figure}$ Figure 12: The sunspot from Sep. 23, 2003, at disk centre in H $\alpha$ (courtesy A. Tritschler, NSO/Sac Peak), showing some indication of vortex structures in the super-penumbra.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2042f13.ps} \end{figure}$ Figure 13: Uppermost panel: azimuthal variation of field inclination ( upper curve), line core intensity of Si 10787 ( middle curve) and field strength ( lower curve) along an azimuthal path at a radial distance of r=0.8 at $\log\tau$ = 0; lower panels: radial variation of the corresponding correlation coefficients for $\log\tau$ = 0 (solid line), -0.5 (dotted), -1.0 (dashed), -2 (dashed-dotted); the umbral-penumbral transition is located at r=0.4-0.5.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f1.ps} \end{figure}$	Figure 1: Maps of the disk centre sunspot from Sep. 23, 2003, showing spectrally integrated Stokes-I, -Q, -U, and -V absolute values.
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$\begin{figure} \par\includegraphics[width=14cm,clip] {2042f3.ps} \end{figure}$	Figure 3: Response functions (RF) of Stokes-I to temperature in a quiet sun atmosphere ( left panels), to LOS velocity in a penumbral atmosphere ( middle panels) and of Stokes-V to magnetic field in a hot umbral atmosphere ( right panels) at different positions throughout the three lines observed.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2042f5.ps} \end{figure}$	Figure 4: Circular paths selected to determine azimuthal means of the deduced parameters.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f8.ps} \end{figure}$	Figure 7: Velocity maps of the disk centre spot at different layers; negative values denote upflows; the contours mark the outer boundary of umbra and penumbra.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f8b.ps} \end{figure}$	Figure 8: Radial variation of azimuthally-averaged LOS velocities retrieved with 5% constant straylight (solid-thick line) and SIR-adapted straylight (dashed-thin line) for different heights. Error bars represent the velocity standard deviations in each radial bin and triangles their extreme values.
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$\begin{figure} \par\mbox{\includegraphics[width=8.3cm,bb=22 3 497 269,clip]{2042... ....ps}\hspace{2mm} \includegraphics[width=8.3cm,clip]{2042f10d.ps} }\end{figure}$	Figure 9: Maps of the vertical ( upper) and the horizontal ( second) components of the magnetic field vector, its inclination ( third) and its azimuth ( lower panel) at 4 different atmospheric height levels marked in each sub-panel. The contours mark the outer boundary of the umbra and of the penumbra.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2042f11.ps} \end{figure}$	Figure 10: Scatter-plots of strength and inclination of the magnetic field for the height levels $\log\tau$ = 0 ( upper left), $\log\tau$ = -0.5 ( upper right), $\log\tau$ = -1.0 ( lower left), and $\log\tau$ = - 2 ( lower right).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip] {2042f9.ps} \end{figure}$	Figure 11: Radial variations of the azimuthally-averaged field azimuth, field strength and field inclination; the latter two are presented for 5% constant straylight and for SIR-adapted straylight. Each sub-figure contains 4 height levels.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip] {2042f12.ps} \end{figure}$	Figure 12: The sunspot from Sep. 23, 2003, at disk centre in H $\alpha$ (courtesy A. Tritschler, NSO/Sac Peak), showing some indication of vortex structures in the super-penumbra.
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