All Figures

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig1.eps}}\end{figure}$ Figure 1: Effective temperature distribution on the surface of a rotating star. The different curves, which are normalized to the polar temperature, are for different rotational velocities indicated by $\omega$ from low values ( upper curves) to high values ( lower curves). In the top panel the rotational distortion of the stellar surface has been neglected.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig2.eps}}\end{figure}$ Figure 2: Distribution of the mass flux ( top panel), the escape velocity ( mid panel), and the hydrogen density ( bottom panel) on the surface of a rotating star. The different curves in each plot, which are normalized to the corresponding polar value of the parameters, are for different rotational velocities indicated by $\omega$ . All parameters drop from pole to equator. This effect becomes stronger with increasing values of $\omega$ .
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig3.eps}}\end{figure}$ Figure 3: Top panel: stellar luminosity as a function of $\omega$ for our model stars with $T_{\rm eff, pole} = 24~500$ K and $R_{*} = 82~R_{\odot}$ . Bottom panel: mass loss rate as a function of $\omega$ , normalized to the spherical mass loss rate. Both parameters show a decrease with increasing rotation speed. The difference between the non-rotating and the critically rotating star is about a factor 2.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig4.eps}}\end{figure}$ Figure 4: Distance r in the equatorial plane in terms of the equatorial radius $R_{\rm eq}(\omega )$ at which recombination of He II ( left panel) and H II ( right panel) takes place for stars rotating with different velocities, indicated by $\omega$ . The curves are ( from top to bottom) for polar mass fluxes of: $F_{\rm m}({\rm pole}) = 1.0\times 10^{-5}$ , $1.5\times 10^{-5}$ and $2.0\times 10^{-5}$ g s^-1 cm^-2.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig5.eps}}\end{figure}$ Figure 5: Surface parameters in the equatorial plane, normalized to their polar values, as functions of the rotational velocity. $n_{\rm H}$ is the density at any distance.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig1.eps}}\end{figure}$	Figure 1: Effective temperature distribution on the surface of a rotating star. The different curves, which are normalized to the polar temperature, are for different rotational velocities indicated by $\omega$ from low values ( upper curves) to high values ( lower curves). In the top panel the rotational distortion of the stellar surface has been neglected.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{5204fig5.eps}}\end{figure}$	Figure 5: Surface parameters in the equatorial plane, normalized to their polar values, as functions of the rotational velocity. $n_{\rm H}$ is the density at any distance.
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