Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[width=16.2cm,clip]{2958fig1.eps} % \end{figure}$ Figure 1: Maps of physical quantities of the snapshots with $\langle B \rangle = 140$ G ( left panels), 30 G ( middle panels) and 10 G (right panels). Upper panels: vertical component of the magnetic field at the level log $\tau _{5000} =0$ , corresponding to the visible solar surface. Middle panels: normalized continuum intensity $\delta I_{\rm c}=(I_{\rm c} -\bar{I_{\rm c}})/\bar{I_{\rm c}}$ at 630 nm. The first two images show local brightenings in the magnetic flux concentrations in intergranular lanes. Lower panels: vertical velocity component, positive values are downflows.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2958fig2.eps}\end{figure}$ Figure 2: Comparison between the averaged synthetic Stokes Iprofiles (solid line) and corresponding observed ones (circles) from the Liège atlas. Upper panel: Fe I 6301 and 6302 Å lines. Lower panel: Fe I 15 648 and 15 652 Å lines.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{2958fig3.eps}\end{figure}$ Figure 3: Left panel: map of the classes of Stokes V profiles of the Fe I 15 648 Å line in the $\langle B\rangle = 30$ G snapshot. Right panels: examples of class profiles (see the discussion in the text). In the left panel green colors mark the locations of the blue-shifted profiles having mostly positive asymmetry (classes d) and e)). Blue and white mark the red-shifted profiles having negative or no asymmetry (classes a) and b)). The yellow and red colors mark the location of the irregularly-shaped profiles (classes c) and f)). The fraction of the profiles belonging to each class is given in percent above each figure. Only profiles with Stokes V amplitudes above 10^-3 are classified.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{2958fig4.eps}\end{figure}$ Figure 4: Left panel: map of the classes of Stokes V profiles of the Fe I 6302 Å line in the $\langle B\rangle = 30$ G snapshot. The color scheme is the same as in Fig. 3. Right panel: examples of the class profiles.
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In the text

$\begin{figure} \par\includegraphics[width=15.85cm,clip]{2958fig5.eps}\end{figure}$ Figure 5: Example of the formation of the irregular Stokes Vprofile belonging to the classes shown in Figs. 3c and 4c. Top panels: distributions of the vertical magnetic field and velocity with optical depth and horizontal distance. The vertical line marks the ray along which the Fe I 15 648 Å and 6302 Å profiles displayed in the middle panels are formed. Bottom panels: the corresponding magnetic field and velocity profiles on the optical depth scale.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{2958fig6.eps}\end{figure}$ Figure 6: Left panel: map of the classes of Stokes V profiles of the Fe I 15 648 Å line in the $\langle B\rangle = 30$ G snapshot. The profiles were smeared to have a resolution of 0 $^{\prime \prime }$ 8 and a contrast $\delta I_{\rm c}=3$ %. Only profiles with amplitudes above 10^-3 are classified. The color coding is the same as in Fig. 3. Right panel: examples of the class profiles. Solid line: class profiles from the simulations; dashed line: class profiles from the quiet Sun observations in the infrared (Khomenko et al. 2003).
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In the text

$\begin{figure} \par\includegraphics[width=15.2cm]{2958fig7.eps}\end{figure}$ Figure 7: Histogram of the amplitudes of Stokes V profiles with original resolution for the $\langle B\rangle$ = 20 and 140 G snapshots (panels $\bf a)$ and $\bf b)$ , respectively). Thick line: Fe I 6302 Å, thin line: Fe I 15 648 Å. The arrows indicate the mean values in both cases.
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{2958fig8.eps}\end{figure}$ Figure 8: Histogram of the amplitudes of Stokes V profiles with reduced resolution for the $\langle B\rangle$ = 10, 20, 30 and 140 G snapshots (panels $\bf a)$ , $\bf b)$ , $\bf c)$ and $\bf d)$ , respectively). Thick line: Fe I 6302; thin line: Fe I 15 648; dotted line: observations in the infrared taken from Khomenko et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{2958fig9.eps}\end{figure}$ Figure 9: Histograms of the amplitude ( top) and area ( bottom) asymmetries of the Stokes V profiles in the $\langle B\rangle=20$ G snapshot at its original resolution. Sold line: all regular-shaped profiles with amplitudes above 10^-3. Dashed line: only profiles in downflowing regions. Dotted line: only profiles in upflowing regions. Left panels: Fe I 15 648 Å, right panels: Fe I 6302 Å. The mean values together with standard deviations corresponding to each curve are given in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{2958fig10.eps}\end{figure}$ Figure 10: Histograms of the amplitude ( top) and area (bottom) asymmetries of the Fe I 6302 Å Stokes V profiles at reduced resolution. All regular-shaped profiles with amplitudes above 10^-3 are considered. Thick line: $\langle B \rangle = 140$ G; thin line: $\langle B\rangle = 30$ G.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{2958fig11.eps}\end{figure}$ Figure 11: Same as Fig. 10 but for Fe I 15 648 Å.
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In the text

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{2958fig12.eps}\end{figure}$ Figure 12: Scatter plots of the Fe I 6302 Å Stokes Vamplitude asymmetry ( left panel) and area asymmetry ( right panel) as a function of Stokes V amplitude in the $\langle B \rangle = 140$ G snapshot.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm]{2958fig13.eps}\vspace*{4mm} \p... ....eps}\vspace*{4mm} \par\includegraphics[width=15.7cm]{2958fig15.eps}\end{figure}$ Figure 13: Simultaneous classification of the Fe I 15 648 Å and Fe I 6302 Å Stokes V profiles in the $\langle B \rangle = 140$ G snapshot. Upper panel: original resolution; middle panel: same amount of smearing at both wavelengths; bottom panel: different amounts of smearing (see text for details). The images show the spatial polarity distribution for both spectral lines. Black and white colors mark the locations of the positive and negative polarity profiles, while grey marks the location of the irregular profiles. To make the comparison easier, only about 2/3 of the original snapshot is shown ( upper right part). The examples of the class profiles corresponding to each classification are given on the right hand side of the figure together with the fraction of the profiles belonging to each class.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2958fig2.eps}\end{figure}$	Figure 2: Comparison between the averaged synthetic Stokes Iprofiles (solid line) and corresponding observed ones (circles) from the Liège atlas. Upper panel: Fe I 6301 and 6302 Å lines. Lower panel: Fe I 15 648 and 15 652 Å lines.
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$\begin{figure} \par\includegraphics[width=15.8cm,clip]{2958fig4.eps}\end{figure}$	Figure 4: Left panel: map of the classes of Stokes V profiles of the Fe I 6302 Å line in the $\langle B\rangle = 30$ G snapshot. The color scheme is the same as in Fig. 3. Right panel: examples of the class profiles.
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$\begin{figure} \par\includegraphics[width=15.2cm]{2958fig7.eps}\end{figure}$	Figure 7: Histogram of the amplitudes of Stokes V profiles with original resolution for the $\langle B\rangle$ = 20 and 140 G snapshots (panels $\bf a)$ and $\bf b)$ , respectively). Thick line: Fe I 6302 Å, thin line: Fe I 15 648 Å. The arrows indicate the mean values in both cases.
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$\begin{figure} \par\includegraphics[width=17cm]{2958fig8.eps}\end{figure}$	Figure 8: Histogram of the amplitudes of Stokes V profiles with reduced resolution for the $\langle B\rangle$ = 10, 20, 30 and 140 G snapshots (panels $\bf a)$ , $\bf b)$ , $\bf c)$ and $\bf d)$ , respectively). Thick line: Fe I 6302; thin line: Fe I 15 648; dotted line: observations in the infrared taken from Khomenko et al. (2003).
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$\begin{figure} \par\includegraphics[width=8cm]{2958fig10.eps}\end{figure}$	Figure 10: Histograms of the amplitude ( top) and area (bottom) asymmetries of the Fe I 6302 Å Stokes V profiles at reduced resolution. All regular-shaped profiles with amplitudes above 10^-3 are considered. Thick line: $\langle B \rangle = 140$ G; thin line: $\langle B\rangle = 30$ G.
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$\begin{figure} \par\includegraphics[width=8cm]{2958fig11.eps}\end{figure}$	Figure 11: Same as Fig. 10 but for Fe I 15 648 Å.
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$\begin{figure} \par\includegraphics[width=14.5cm,clip]{2958fig12.eps}\end{figure}$	Figure 12: Scatter plots of the Fe I 6302 Å Stokes Vamplitude asymmetry ( left panel) and area asymmetry ( right panel) as a function of Stokes V amplitude in the $\langle B \rangle = 140$ G snapshot.
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