All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg1.eps}\end{figure}$ Figure 1: A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is the model computed with ATLAS_ODF and the dashed line is the solar model atmosphere asunodfnew.dat from the Kurucz web page. The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure. The differences are entirely due to the conversion to Fortran 2003 and to using consistent, modern values of fundamental parameters throughout the ATLAS_ODF code. The numerical methods are the same for the two models.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg2.eps}\end{figure}$ Figure 2: A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is for the model computed with ATLAS_OS and the dashed line is the model computed with ATLAS_ODF. The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure. The differences are entirely due to the way in which line opacity is included. Both codes use Fortran 2003, the same fundamental parameters and the same numerical methods.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg3.eps}\end{figure}$ Figure 3: A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperature as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is the model computed with ATLAS_OS, and the dashed line is an ATLAS12 model provided by Kurucz (private communication). The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg4.eps}\end{figure}$ Figure 4: The geometry used for the Rybicki (1971) method of radiative transfer. The rays are distributed over the core in equal steps of 0.1 in $\mu$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0578fg5.eps}\end{figure}$ Figure 5: A comparison of the temperature structures for two solar atmospheric models, both using the ATLAS_ODF code. The solid line used the Rybicki (1971) method to compute the radiative transfer, and the dashed line used the original ATLAS9 integral equation method.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg6.eps}\end{figure}$ Figure 6: A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is computed using spherical geometry and the dashed line is using the traditional plane-parallel geometry. The radiative transfer and the pressure structures of both models were computed using the same numerical techniques. The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg7.eps}\end{figure}$ Figure 7: A comparison of the temperature structures of two red giant atmospheric models. The top panel displays the temperatures as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is a spherical model with the parameters $L = 3690~L_{\hbox{$\odot$ }}$ , $M = 1~M_{\hbox{$\odot$ }}$ and $R = 166~R_{\hbox{$\odot$ }}$ . These values were chosen to match the parameters of the plane-parallel model having $T_{{\rm eff}} = 3500$ K and $\log g = 0.0$ , computed using ATLAS_ODF, shown by the dashed line. The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg8.eps}\end{figure}$ Figure 8: A comparison of the structures of two spherical red giant atmospheric models, both equivalent to $T_{{\rm eff}} = 3500$ K and $\log g = 0.0$ . The top panel displays the temperatures as a function of $\log_{10} (P_{{\rm gas}})$ . The solid line is a spherical model having $L = 3690~L_{\hbox{$\odot$ }}$ , $M = 1~M_{\hbox{$\odot$ }}$ and $R = 166~R_{\hbox{$\odot$ }}$ . The dashed line, which is nearly coincident with the solid line, represents the model having the parameters $L = 2952~L_{\hbox{$\odot$ }}$ , $M = 0.8~M_{\hbox{$\odot$ }}$ and $R = 148~R_{\hbox{$\odot$ }}$ . The bottom panel shows the percentage difference between the temperatures of the two models, also as a function of the gas pressure. The sense of the differences is the less massive and luminous model minus the more massive and luminous model.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg9.eps}\vspace*{2mm} \end{figure}$ Figure 9: A comparison of the temperature structures of an SATLAS_ODF atmosphere (solid line) with the structure of a model from the NG-giant grid computed with the PHOENIX code (dashed line). The SATLAS model has the atmospheric parameters $L = 10~324~L_{\hbox{$\odot$ }}$ , $M = 2.5~M_{\hbox{$\odot$ }}$ and $R = 262~R_{\hbox{$\odot$ }}$ , corresponding to the NextGen parameters $T_{{\rm eff}} = 3600$ K, $\log g = 0.0$ and $M = 2.5~M_{\hbox{$\odot$ }}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg10.eps} \end{figure}$ Figure 10: A comparison of the temperature structures of an SATLAS_ODF atmosphere (solid line) with a spherical MARCS model (dashed line). The SATLAS model has the atmospheric parameters $L = 6390~L_{\hbox{$\odot$ }}$ , $M = 1.0~M_{\hbox{$\odot$ }}$ and $R = 166~R_{\hbox{$\odot$ }}$ , corresponding to the MARCS parameters $T_{{\rm eff}} = 4000$ K, $\log g = 0.0$ and $M = 1.0~M_{\hbox{$\odot$ }}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0578fg4.eps}\end{figure}$	Figure 4: The geometry used for the Rybicki (1971) method of radiative transfer. The rays are distributed over the core in equal steps of 0.1 in $\mu$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0578fg5.eps}\end{figure}$	Figure 5: A comparison of the temperature structures for two solar atmospheric models, both using the ATLAS_ODF code. The solid line used the Rybicki (1971) method to compute the radiative transfer, and the dashed line used the original ATLAS9 integral equation method.
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