All Figures

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F1.eps}}\end{figure}$ Figure 1: Angular distribution of the mass flux, velocity and hydrogen density on the stellar surface. The parameters are b₁ = 1; b₂ = -2; s = 100 (dashed lines); b₁ = 0.5; b₂ = -1.5; s = 100 (dotted lines); and b₁ = 1; b₂ = -2; s = 10 (solid lines).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F2.eps}}\end{figure}$ Figure 2: Hydrogen and helium recombination coefficients. The dots for H refer to values given by Seaton (1959), the dots for He are taken from Osterbrock (1989), and the lines give fits according to interpolation calculations.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F3.eps}}\end{figure}$ Figure 3: Ionization radii in equatorial regions of H (dashed lines) and He (solid lines) for the different model calculations in the optically thin approximation. The stellar surface is shown as the dotted line.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F4.eps}}\end{figure}$ Figure 4: As in Fig. 3 but for the on-the-spot approximation.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F5.eps}}\end{figure}$ Figure 5: Optically thin approximation for the models D and E but for a much larger distance. Shown are the ionization radii for H (dashed line) and He (solid line).
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F6.eps}}\end{figure}$ Figure 6: On-the-spot approximation for the models D and E but for a much larger distance. Shown are the ionization radii for H (dashed line) and He (solid line).
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{H4034F7.eps}}\end{figure}$ Figure 7: He ionization structure in equatorial direction ( $\theta = 90\hbox {$^\circ $ }$ ) for the different models. The models are grouped according to their density in equatorial direction: the upper panel belongs to the highest density, the lower panel to the lowest density models. The shift of the transition radius to higher distances for lower densities is clearly visible. The solid lines represent $q_{\rm He^{+}}$ and the dashed lines $q_{\rm He^{0}} = 1 - q_{\rm He^{+}}$ . The thick vertical line is the location of the ionization radius from Fig. 4.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{H4034F8.eps}}\end{figure}$ Figure 8: As Fig. 7 but for the H ionization structure. Models D and E are not shown because due to their low densities no transition from ionized to neutral occurs; the ionization fraction in these winds becomes constant.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F1.eps}}\end{figure}$	Figure 1: Angular distribution of the mass flux, velocity and hydrogen density on the stellar surface. The parameters are b₁ = 1; b₂ = -2; s = 100 (dashed lines); b₁ = 0.5; b₂ = -1.5; s = 100 (dotted lines); and b₁ = 1; b₂ = -2; s = 10 (solid lines).
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F2.eps}}\end{figure}$	Figure 2: Hydrogen and helium recombination coefficients. The dots for H refer to values given by Seaton (1959), the dots for He are taken from Osterbrock (1989), and the lines give fits according to interpolation calculations.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F3.eps}}\end{figure}$	Figure 3: Ionization radii in equatorial regions of H (dashed lines) and He (solid lines) for the different model calculations in the optically thin approximation. The stellar surface is shown as the dotted line.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F4.eps}}\end{figure}$	Figure 4: As in Fig. 3 but for the on-the-spot approximation.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F5.eps}}\end{figure}$	Figure 5: Optically thin approximation for the models D and E but for a much larger distance. Shown are the ionization radii for H (dashed line) and He (solid line).
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{H4034F6.eps}}\end{figure}$	Figure 6: On-the-spot approximation for the models D and E but for a much larger distance. Shown are the ionization radii for H (dashed line) and He (solid line).
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{H4034F8.eps}}\end{figure}$	Figure 8: As Fig. 7 but for the H ionization structure. Models D and E are not shown because due to their low densities no transition from ionized to neutral occurs; the ionization fraction in these winds becomes constant.
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