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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4188.fig1}\end{figure}$ Figure 1: Different solutions of the momentum equation for the stellar parameters of an O5IV star (see Table 1) rotating at $v_{\rm eq}=300$ km s^-1. The solutions for increasing mass-loss rates are indicated as full lines. The dashed-dot line indicates graphically that the momentum equation is no longer solvable for the indicated and higher mass-loss rates.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.1cm,clip]{H4188.fig2a}\hspace*{3mm} \includegraphics[angle=270,width=8.1cm,clip]{H4188.fig2b}\end{figure}$ Figure 2: Different solutions of the momentum equation for the stellar parameters of an O5IV star (see Table 1) rotating at $v_{\rm eq}=500$ km s^-1. Left panel: solutions with increasing velocities towards infinity are indicated as full lines; the dashed lines are solutions for which the line force is exhausted at a certain distance. The dashed-dot line indicates graphically that the momentum equation is no longer solvable for the indicated and higher mass-loss rates. Right: selected solutions giving the transition from infinitely increasing to decreasing velocity laws. The thick vertical line segment indicates the position at which line driving is no longer effective.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{H4188.fig3a}\hspace*{2mm} \includegraphics[angle=270,width=8.5cm,clip]{H4188.fig3b}\end{figure}$ Figure 3: Same as Fig. 2, but for a B5II star rotating at $v_{\rm eq}=400~$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{betawet.eps}\end{figure}$ Figure 4: A comparison between a velocity law found from Eq. (9) (dashed line) and different $\beta$ velocity laws (full lines). The latter are drawn for $\beta =0.1$ (upper curve) $\rightarrow$ 1.9 (lower curve) in steps of 0.2.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{H4188.fig4a}\hspace*{2mm} \includegraphics[angle=270,width=8.5cm,clip]{H4188.fig4b}\end{figure}$ Figure 5: Left panel: the velocity law for the O5IV star having $v_{\rm eq}=500~$ km s^-1 and $\dot{M}_{\rm eq}=4.0 \times 10^{-6}~M_\odot$ yr^-1. Full line: inclusion of finite disk correction. Dashed line: neglect of finite disk correction. Dotted line: same as dashed line, but for $\dot{M}_{\rm eq}=3.9 \times 10^{-6}~M_\odot$ yr^-1. Right panel: same as left panel but for the velocity law of the B5II star having $v_{\rm eq}=400~$ km s^-1 and $\dot{M}_{\rm eq}=0.8 \times 10^{-6}~M_\odot$ yr^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4188.fig5}\end{figure}$ Figure 6: The velocity law for the O5IV star having $v_{\rm eq}=500~$ km s^-1 and $\dot{M}_{\rm eq}=4$ $\times$ $10^{-6}~M_\odot$ yr^-1 with the inclusion of finite disk correction. The sonic point was fixed at $1.1~R_\star$ (full line) and at $1.01~R_\star$ (dashed line).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4188.fig1}\end{figure}$	Figure 1: Different solutions of the momentum equation for the stellar parameters of an O5IV star (see Table 1) rotating at $v_{\rm eq}=300$ km s^-1. The solutions for increasing mass-loss rates are indicated as full lines. The dashed-dot line indicates graphically that the momentum equation is no longer solvable for the indicated and higher mass-loss rates.
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$\begin{figure} \par\includegraphics[angle=270,width=8.3cm,clip]{H4188.fig3a}\hspace*{2mm} \includegraphics[angle=270,width=8.5cm,clip]{H4188.fig3b}\end{figure}$	Figure 3: Same as Fig. 2, but for a B5II star rotating at $v_{\rm eq}=400~$ km s^-1.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{betawet.eps}\end{figure}$	Figure 4: A comparison between a velocity law found from Eq. (9) (dashed line) and different $\beta$ velocity laws (full lines). The latter are drawn for $\beta =0.1$ (upper curve) $\rightarrow$ 1.9 (lower curve) in steps of 0.2.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4188.fig5}\end{figure}$	Figure 6: The velocity law for the O5IV star having $v_{\rm eq}=500~$ km s^-1 and $\dot{M}_{\rm eq}=4$ $\times$ $10^{-6}~M_\odot$ yr^-1 with the inclusion of finite disk correction. The sonic point was fixed at $1.1~R_\star$ (full line) and at $1.01~R_\star$ (dashed line).
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