All Figures

$\begin{figure} \par\includegraphics[width=9cm,clip]{9885fig1.eps}\end{figure}$ Figure 1: Comparison of the temperature structures of the CO⁵BOLD model used in this work, the 3D model of A04, and the Holweger-Müller model. For the 3D models the RMS fluctuations (thin lines) around the mean (thick lines) are indicated.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[draft = false] {9885fig2.eps}}\end{figure}$ Figure 2: The equivalent width contribution function, dEW/d $\log \tau$ , for the 777.1 nm line at disc-centre, calculated from the 3D model (solid line), the $\ensuremath{\left\langle{\rm 3D}\right\rangle}$ model (triple dot-dashed), and the $\ensuremath {{\rm 1D}_{{\rm LHD}}}$ model (dashed). Following Magain (1986), the contribution function is defined such that integration over $\log\tau_\lambda$ gives the line equivalent width.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig3.eps}}\end{figure}$ Figure 3: The four observed spectra we used for the analysis of the [O I] 630 nm line. The Kurucz flux spectrum, KF, and the Neckel flux, NF, and Neckel intensity, NI, spectra plotted here are the normalised spectra provided by Kurucz (2005a) and Neckel (1999); the NI is shifted up by 0.1 for clarity, while the Delbouille intensity, DI, has been normalised and then shifted up by 0.1. The vertical line indicates the laboratory wavelength of the oxygen line. We recall that KF is corrected for gravitational redshift while NF is not, explaining the large wavelength differences between the two flux atlases.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig4.eps}}\end{figure}$ Figure 4: The contribution of Ni I line (dashed line) with A(Ni) = 6.25 is compared to the combined [O I]+Ni I blend (solid line) for disc-centre according to the Linfor3D computation with A(O) = 8.66.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig5.eps}}\end{figure}$ Figure 5: The 3D fit of the [OI] 630 nm line. The observed spectra (diamonds, their size indicating the observational noise level) are superimposed on the best fit 3D synthetic line profile (solid). From top to bottom, the spectra are: Delbouille intensity (DI), Neckel intensity (NI), Neckel flux (NF), and Kurucz flux (KF).
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig6.eps}}\end{figure}$ Figure 6: The Kurucz flux spectrum around the [OI] 636.378 nm line with the identification of the stronger lines.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig7.eps}}\end{figure}$ Figure 7: The O I 615 nm Mult. 10 lines in the four observed spectra used in this work. Symbols are as in Fig. 3. The three vertical lines indicate the laboratory wavelength of the lines.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig8.eps}}\end{figure}$ Figure 8: The average temperature profile (left ordinate) of the 3D model (solid line) and the temperature profile of the $\ensuremath {{\rm 1D}_{{\rm LHD}}}$ model (dashed) are depicted as a function of Rosseland optical depth. The EW contribution function of the disc-centre 3D synthetic spectrum (right ordinate) of the 615 nm line (solid), is compared to that of the 630 nm (dashed) and 777 nm (triple dot-dashed) lines. The contribution functions are scaled to have similar maxima and are plotted against their respective monochromatic continuum optical depths.
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In the text

$\begin{figure} \par\includegraphics[clip=15cm,clip]{9885fig9.eps}\end{figure}$ Figure 9: The O I 777 nm triplet in the four observed spectra used in this work. Symbols are as for Fig. 3.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig10.eps}}\end{figure}$ Figure 10: The O I 844 nm line in the four observed spectra used in this work. Symbols are as for Fig. 3. The vertical line indicates the laboratory wavelength position of the line.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig11.eps}}\end{figure}$ Figure 11: The observed Delbouille (DI) and Wallace (WI) disc-centre intensity spectra of the O I 926 nm line.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig12.eps}}\end{figure}$ Figure 12: The observed disc-centre intensity spectrum used for the O I 1130 nm line. The vertical line indicates the laboratory wavelength position of the line.
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In the text

$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig13.eps}}\end{figure}$ Figure 13: The observed disc-centre intensity spectrum used for the analysis of the O I 1316 nm line. The vertical lines indicate the laboratory wavelengths of the three O I lines discussed in the text.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9885fig1.eps}\end{figure}$	Figure 1: Comparison of the temperature structures of the CO⁵BOLD model used in this work, the 3D model of A04, and the Holweger-Müller model. For the 3D models the RMS fluctuations (thin lines) around the mean (thick lines) are indicated.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig4.eps}}\end{figure}$	Figure 4: The contribution of Ni I line (dashed line) with A(Ni) = 6.25 is compared to the combined [O I]+Ni I blend (solid line) for disc-centre according to the Linfor3D computation with A(O) = 8.66.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig5.eps}}\end{figure}$	Figure 5: The 3D fit of the [OI] 630 nm line. The observed spectra (diamonds, their size indicating the observational noise level) are superimposed on the best fit 3D synthetic line profile (solid). From top to bottom, the spectra are: Delbouille intensity (DI), Neckel intensity (NI), Neckel flux (NF), and Kurucz flux (KF).
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig6.eps}}\end{figure}$	Figure 6: The Kurucz flux spectrum around the [OI] 636.378 nm line with the identification of the stronger lines.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig7.eps}}\end{figure}$	Figure 7: The O I 615 nm Mult. 10 lines in the four observed spectra used in this work. Symbols are as in Fig. 3. The three vertical lines indicate the laboratory wavelength of the lines.
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$\begin{figure} \par\includegraphics[clip=15cm,clip]{9885fig9.eps}\end{figure}$	Figure 9: The O I 777 nm triplet in the four observed spectra used in this work. Symbols are as for Fig. 3.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig10.eps}}\end{figure}$	Figure 10: The O I 844 nm line in the four observed spectra used in this work. Symbols are as for Fig. 3. The vertical line indicates the laboratory wavelength position of the line.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig11.eps}}\end{figure}$	Figure 11: The observed Delbouille (DI) and Wallace (WI) disc-centre intensity spectra of the O I 926 nm line.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig12.eps}}\end{figure}$	Figure 12: The observed disc-centre intensity spectrum used for the O I 1130 nm line. The vertical line indicates the laboratory wavelength position of the line.
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$\begin{figure} \resizebox{9cm}{!}{\includegraphics[clip=true,angle=0]{9885fig13.eps}}\end{figure}$	Figure 13: The observed disc-centre intensity spectrum used for the analysis of the O I 1316 nm line. The vertical lines indicate the laboratory wavelengths of the three O I lines discussed in the text.
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