All Figures

$\begin{figure} \par\includegraphics[width=6cm,clip]{5521_01.eps}\end{figure}$ Figure 1: Radius is plotted over optical depth. The optical depth was calculated from the wavelength independent continuous opacity. The atmosphere is about 60 m thick, but the layers with an optical depth around one lie just centimeters below the outermost layer.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_02.eps}\end{figure}$ Figure 2: Results for non-scattering model line and continuum.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_03.eps}\end{figure}$ Figure 3: The model line and the continuum are scattering with $\epsilon _{\rm line} = 0.01$ and $\epsilon _\kappa = 0.01$ respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_04.eps}\end{figure}$ Figure 4: The model line scatters with $\epsilon _{\rm line} = 0.01$ while the continuum scattering factor is $\epsilon _\kappa = 1.0$ $\times$ 10^-6.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_05.eps}\end{figure}$ Figure 5: The model line is nonscattering with a completely scattering - $\epsilon _\kappa = 0$ - continuum.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_06.eps}\end{figure}$ Figure 6: The model line is completely scattering - $\epsilon _{\rm line} = 0$ - while the continuum is not scattering at all.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_07.eps}\end{figure}$ Figure 7: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 1$ . The blackbody fits the model reasonably well.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_08.eps}\end{figure}$ Figure 8: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 0.1$ The blackbody doesn't fit the model spectrum. The apparent temperature is higher than the model temperature.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_09.eps}\end{figure}$ Figure 9: The model spectrum is the same as in Fig. 8, but this time the temperature of the blackbody was chosen to fit the spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_10.eps}\end{figure}$ Figure 10: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 0.001$ The blackbody doesn't fit the model spectrum. The apparent temperature is higher than the model temperature.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_11.eps}\end{figure}$ Figure 11: The model spectrum is the same as in Fig. 10, but this time the temperature of the blackbody was chosen to fit the spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{5521_12.eps}\end{figure}$ Figure 12: Thermalisation depth is plotted over optical depth. Since the radial structure is only known on a discrete grid the value of the thermalisation depth for a given temperature was determined via linear interpolation.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{5521_01.eps}\end{figure}$	Figure 1: Radius is plotted over optical depth. The optical depth was calculated from the wavelength independent continuous opacity. The atmosphere is about 60 m thick, but the layers with an optical depth around one lie just centimeters below the outermost layer.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_02.eps}\end{figure}$	Figure 2: Results for non-scattering model line and continuum.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_03.eps}\end{figure}$	Figure 3: The model line and the continuum are scattering with $\epsilon _{\rm line} = 0.01$ and $\epsilon _\kappa = 0.01$ respectively.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_04.eps}\end{figure}$	Figure 4: The model line scatters with $\epsilon _{\rm line} = 0.01$ while the continuum scattering factor is $\epsilon _\kappa = 1.0$ $\times$ 10^-6.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_05.eps}\end{figure}$	Figure 5: The model line is nonscattering with a completely scattering - $\epsilon _\kappa = 0$ - continuum.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{5521_06.eps}\end{figure}$	Figure 6: The model line is completely scattering - $\epsilon _{\rm line} = 0$ - while the continuum is not scattering at all.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_07.eps}\end{figure}$	Figure 7: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 1$ . The blackbody fits the model reasonably well.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_08.eps}\end{figure}$	Figure 8: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 0.1$ The blackbody doesn't fit the model spectrum. The apparent temperature is higher than the model temperature.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_09.eps}\end{figure}$	Figure 9: The model spectrum is the same as in Fig. 8, but this time the temperature of the blackbody was chosen to fit the spectrum.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_10.eps}\end{figure}$	Figure 10: The spectrum was corrected for the gravitational redshift and fitted with a blackbody with the known effective temperature of the model - $T_{{\rm eff}}= 10^4$ K. The continuum has $\epsilon _\kappa = 0.001$ The blackbody doesn't fit the model spectrum. The apparent temperature is higher than the model temperature.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{5521_11.eps}\end{figure}$	Figure 11: The model spectrum is the same as in Fig. 10, but this time the temperature of the blackbody was chosen to fit the spectrum.
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$\begin{figure} \par\includegraphics[width=6.3cm,clip]{5521_12.eps}\end{figure}$	Figure 12: Thermalisation depth is plotted over optical depth. Since the radial structure is only known on a discrete grid the value of the thermalisation depth for a given temperature was determined via linear interpolation.
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