All Figures

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F1.eps} }\end{figure}$ Figure 1: The SED for the single-annulus test case nr. A1 (Herbig Ae star) at 1 AU, compared to the CG⁺ model in its two proposed variants.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F2.eps} }\end{figure}$ Figure 2: The temperature structure for the single-annulus test case A1 (Herbig Ae star), compared to the CG⁺ model in its two proposed variants. The transition from the surface to the midplane temperature in the CG⁺ models occurs at $H_{\rm s}$ , i.e., where the optical depth along a ray at a grazing angle $\alpha =0.05$ at stellar wavelengths is $\tau _\ast \sim 1$ . The tick mark on the solid curve shows the location of $H_{\rm s}$ in the 1+1D case.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F3.eps} }\end{figure}$ Figure 3: The SED for the single-annulus test case No. A2 (T Tauri star) at 1 AU, compared to the CG⁺ model in its two proposed variants.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F4.eps} }\end{figure}$ Figure 4: The SED for the single-annulus test case No. A3 (Herbig Ae star, high optical depth) at 50 AU, compared to the CG⁺ model in its two proposed variants.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F5.eps} }\end{figure}$ Figure 5: The temperature structure for model A3.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F6.eps} }\end{figure}$ Figure 6: The SED for the full disk model F1 (Herbig Ae star), compared to the CG⁺ model in its two proposed variants.
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In the text

$\begin{figure} { \includegraphics[width=9cm]{3618F7.eps} }\end{figure}$ Figure 7: Same as Fig. 6, but now for model F2 (a T Tauri star).
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In the text

$\begin{figure} { \includegraphics[width=9cm]{3618F8.eps} }\end{figure}$ Figure 8: Same as Fig. 6, but now for model F3 (a Brown Dwarf).
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F9a.eps} } \vspace*{2mm} { \includegraphics[width=8.8cm,clip]{3618F9b.eps} }\end{figure}$ Figure 9: Top panel: pressure scale height $H_{\rm p}$ and surface height $H_{\rm s}$ as function of R for model F1 (Herbig Ae star). The solid line shows the results of the vertical structure model, the dashed line those of CG⁺ ones. Bottom Panel: same for model F2 (T Tauri star).
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In the text

$\begin{figure} { \includegraphics[width=8.8cm]{figure_10.ps} }%\end{figure}$ Figure 10: The flaring index of the disk $\xi$ is plotted as a function of radius for model F2 (T Tauri star). The vertical structure model is shown as a solid line, while the CG⁺ is the dashed line.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F11.eps} }\end{figure}$ Figure 11: The brightness profile of model F2 (T Tauri star) as a function of radius at two different wavelengths. The 1+1D model results are shown as a solid line, the CG⁺ model results as a dashed line.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F12.eps} }\end{figure}$ Figure 12: Example of the effect of scattering on the SED of a T Tauri disk (model F3). Only the thermal emission of the disk is shown in this figure. Scattered light would appear as a strong rise towards short wavelengths.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F13a.eps} } \vspace*{2mm} { \includegraphics[width=8.8cm,clip]{3618F13b.eps} }\end{figure}$ Figure 13: The factor by which scattering suppresses the SED of the disk annulus of test cases A1 and A2 for an albedo of $\omega =0.5$ . The solid line is the suppression factor from the 1D vertical structure model. The other lines are for the two recipes proposed for the CG⁺ model.
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In the text

$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F1.eps} }\end{figure}$	Figure 1: The SED for the single-annulus test case nr. A1 (Herbig Ae star) at 1 AU, compared to the CG⁺ model in its two proposed variants.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F3.eps} }\end{figure}$	Figure 3: The SED for the single-annulus test case No. A2 (T Tauri star) at 1 AU, compared to the CG⁺ model in its two proposed variants.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F4.eps} }\end{figure}$	Figure 4: The SED for the single-annulus test case No. A3 (Herbig Ae star, high optical depth) at 50 AU, compared to the CG⁺ model in its two proposed variants.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F5.eps} }\end{figure}$	Figure 5: The temperature structure for model A3.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F6.eps} }\end{figure}$	Figure 6: The SED for the full disk model F1 (Herbig Ae star), compared to the CG⁺ model in its two proposed variants.
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$\begin{figure} { \includegraphics[width=9cm]{3618F7.eps} }\end{figure}$	Figure 7: Same as Fig. 6, but now for model F2 (a T Tauri star).
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$\begin{figure} { \includegraphics[width=9cm]{3618F8.eps} }\end{figure}$	Figure 8: Same as Fig. 6, but now for model F3 (a Brown Dwarf).
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F9a.eps} } \vspace*{2mm} { \includegraphics[width=8.8cm,clip]{3618F9b.eps} }\end{figure}$	Figure 9: Top panel: pressure scale height $H_{\rm p}$ and surface height $H_{\rm s}$ as function of R for model F1 (Herbig Ae star). The solid line shows the results of the vertical structure model, the dashed line those of CG⁺ ones. Bottom Panel: same for model F2 (T Tauri star).
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$\begin{figure} { \includegraphics[width=8.8cm]{figure_10.ps} }%\end{figure}$	Figure 10: The flaring index of the disk $\xi$ is plotted as a function of radius for model F2 (T Tauri star). The vertical structure model is shown as a solid line, while the CG⁺ is the dashed line.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F11.eps} }\end{figure}$	Figure 11: The brightness profile of model F2 (T Tauri star) as a function of radius at two different wavelengths. The 1+1D model results are shown as a solid line, the CG⁺ model results as a dashed line.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F12.eps} }\end{figure}$	Figure 12: Example of the effect of scattering on the SED of a T Tauri disk (model F3). Only the thermal emission of the disk is shown in this figure. Scattered light would appear as a strong rise towards short wavelengths.
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$\begin{figure} { \includegraphics[width=8.8cm,clip]{3618F13a.eps} } \vspace*{2mm} { \includegraphics[width=8.8cm,clip]{3618F13b.eps} }\end{figure}$	Figure 13: The factor by which scattering suppresses the SED of the disk annulus of test cases A1 and A2 for an albedo of $\omega =0.5$ . The solid line is the suppression factor from the 1D vertical structure model. The other lines are for the two recipes proposed for the CG⁺ model.
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