All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f1.eps}\end{figure}$ Figure 1: Temperature distribution in atmospheres of $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ , and various chemical compositions. Both Compton and Thomson scattering models are shown here. The solid line represents an atmosphere with solar iron abundance $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-5 and the dashed line represents a model with the iron abundance 100 times higher (Compton scattering models). Dotted line: model with solar iron abundance, long dashed line - 100 times higher iron abundance (Thomson scattering).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f2.eps}\end{figure}$ Figure 2: Temperature stratification in atmospheres of $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ , and different iron abundances. Solid line - solar abundance of iron, $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-5, dotted line - iron abundance is 100 times higher; dashed line - H-He atmosphere.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f3.eps}\end{figure}$ Figure 3: Temperature structure of atmospheres at the fixed $T_{{\rm eff}}=2$ $\times$ 10⁷ K and solar iron abundance, and different surface gravities. Solid line - $\log{g}=14.1$ , dashed line - 14.3, dotted line - 14.5, dot-dashed line - 14.9.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f4.eps}\end{figure}$ Figure 4: Temperature structure of atmospheres with solar iron abundance and $\log{g}=14.5$ , and of different $T_{{\rm eff}}$ ; solid line - model of $T_{{\rm eff}}=10^7$ K, dotted line - 1.5 $\times$ 10⁷ K.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f5.eps}\end{figure}$ Figure 5: Fractional abundances for various iron ions in the atmosphere with $T_{{\rm eff}}=10^7$ K, $\log{g}=14.5$ , and the solar iron abundance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f6.eps}\end{figure}$ Figure 6: Comparison of outgoing spectra computed either with Thomson scattering or Compton scattering, and the blackbody spectrum. All model spectra displayed here are computed with $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{f7.eps}\end{figure}$ Figure 7: Outgoing flux spectra of the atmosphere of $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ , and different iron abundances. Long dashed line - model with $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-3, solid line - solar iron abundance $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-5, dotted line - H-He atmosphere, dashed line - blackbody spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{f8.eps}\end{figure}$ Figure 8: Flux spectra for $T_{{\rm eff}}=10^7$ K and $\log g=12.9$ , and different chemical composition. Solid line - model with iron abundance 100 times solar value, dashed line - the blackbody spectrum, dotted line - model spectrum of pure H-He atmosphere.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f9.eps}\end{figure}$ Figure 9: Comparison of theoretical spectra of atmospheres with different $\log g$ and fixed $T_{{\rm eff}}=2$ $\times$ 10⁷ K and solar iron abundance. Solid line - $\log{g}=14.1$ (it is very close to the Eddington limit), dotted line - 14.3, dashed line - 14.5, long dashed line - 14.7, and the dot-dashed line - 14.9.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f10.eps}\end{figure}$ Figure 10: Run of ratios $T_{\rm c}/T_{{\rm eff}}$ vs. $\log g$ in models with solar iron abundance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f11.eps}\end{figure}$ Figure 11: Run of ratios $T_{\rm c}/T_{{\rm eff}}$ vs. $\log g$ in models with iron abundance 100 times higher than the solar value.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f2.eps}\end{figure}$	Figure 2: Temperature stratification in atmospheres of $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ , and different iron abundances. Solid line - solar abundance of iron, $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-5, dotted line - iron abundance is 100 times higher; dashed line - H-He atmosphere.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f3.eps}\end{figure}$	Figure 3: Temperature structure of atmospheres at the fixed $T_{{\rm eff}}=2$ $\times$ 10⁷ K and solar iron abundance, and different surface gravities. Solid line - $\log{g}=14.1$ , dashed line - 14.3, dotted line - 14.5, dot-dashed line - 14.9.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f4.eps}\end{figure}$	Figure 4: Temperature structure of atmospheres with solar iron abundance and $\log{g}=14.5$ , and of different $T_{{\rm eff}}$ ; solid line - model of $T_{{\rm eff}}=10^7$ K, dotted line - 1.5 $\times$ 10⁷ K.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{f5.eps}\end{figure}$	Figure 5: Fractional abundances for various iron ions in the atmosphere with $T_{{\rm eff}}=10^7$ K, $\log{g}=14.5$ , and the solar iron abundance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f6.eps}\end{figure}$	Figure 6: Comparison of outgoing spectra computed either with Thomson scattering or Compton scattering, and the blackbody spectrum. All model spectra displayed here are computed with $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{f7.eps}\end{figure}$	Figure 7: Outgoing flux spectra of the atmosphere of $T_{{\rm eff}}=2$ $\times$ 10⁷ K and $\log{g}=14.5$ , and different iron abundances. Long dashed line - model with $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-3, solid line - solar iron abundance $N_{{\rm Fe}}/N_{\rm H} = 3.7$ $\times$ 10^-5, dotted line - H-He atmosphere, dashed line - blackbody spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{f8.eps}\end{figure}$	Figure 8: Flux spectra for $T_{{\rm eff}}=10^7$ K and $\log g=12.9$ , and different chemical composition. Solid line - model with iron abundance 100 times solar value, dashed line - the blackbody spectrum, dotted line - model spectrum of pure H-He atmosphere.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f9.eps}\end{figure}$	Figure 9: Comparison of theoretical spectra of atmospheres with different $\log g$ and fixed $T_{{\rm eff}}=2$ $\times$ 10⁷ K and solar iron abundance. Solid line - $\log{g}=14.1$ (it is very close to the Eddington limit), dotted line - 14.3, dashed line - 14.5, long dashed line - 14.7, and the dot-dashed line - 14.9.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f10.eps}\end{figure}$	Figure 10: Run of ratios $T_{\rm c}/T_{{\rm eff}}$ vs. $\log g$ in models with solar iron abundance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{f11.eps}\end{figure}$	Figure 11: Run of ratios $T_{\rm c}/T_{{\rm eff}}$ vs. $\log g$ in models with iron abundance 100 times higher than the solar value.
Open with DEXTER