All Figures

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0325fig1.eps} \end{figure}$ Figure 1: a) The function $\gamma$ versus $r/R_{\ast }-1$ (Eq. (54)) for different values of the rotational parameter $\Omega$ . $\Omega =0$ , continuous-line; $\Omega =0.25$ , dashed-line; $\Omega =0.8$ , dotted-line. The horizontal line is for $\gamma =0$ . b) The eigenvalue from Eq. (48) as a function of $r/R_{\ast }-1$ for the same values of $\Omega$ as a). Note that ${\rm d}\bar{C}/{\rm d}u$ is always negative in the interval $(r_{\rm min},r_{\rm max})$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0325fig2.eps} \end{figure}$ Figure 2: The topology of the freeze in ionization rotating-CAK model ( ${\delta =0}$ ), p versus $(r/R_{\ast }-1)$ for $\Omega =0.25$ . The unique curve that starts at the stellar surface and reaches infinity is the CAK original solution (continuous-line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0325fig3.eps}\par \end{figure}$ Figure 3: The velocity profile v(r) (in km s^-1) as function of $r/R_{\ast }-1$ for the non rotating case (continuous-line) and for the rotational cases: $\Omega =0.25$ dashed-line; $\Omega =0.8$ dotted-line. The location of the singular points is indicated by a larger-dot.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0325fig4.eps} \end{figure}$ Figure 4: Same as Figs. 1a and b but for $\delta =0.02$ . See text for discussion.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0325fig5.eps} \end{figure}$ Figure 5: The velocity profile v(r) (in km s^-1) as function of $r/R_{\ast }-1$ for the non rotating case (continuous-line) and for the rotational cases: $\Omega =0.25$ dashed-line; $\Omega =0.8$ dotted-line.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0325fig6.eps} \end{figure}$ Figure 6: The curves $r_{\rm min}$ and $r_{\pm }$ are shown with continuous lines as function of $\Omega$ . These curves represent the boundaries for the type of the singular point topology. The numerical results for the location of the singular point is also shown in dashed-line. a) is for $\delta =0.02$ and b) for $\delta =0.1$ . See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0325fig7.eps} \end{figure}$ Figure 7: The topology of the rotating-CAK model, p versus $r/R_{\ast }-1$ for $\Omega =0.25$ and $\delta =0.02$ . The unique curve that starting at the stellar surface and reaches infinity is the CAK original solution (continuous-line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0325fig8.eps} \end{figure}$ Figure 8: The topology of the rotating-CAK model, p versus $(r/R_{\ast }-1)$ for $\Omega =0.25$ . The different curves correspond to different values of the eigenvalues. The left-most curve starts at the "normal'' critical point and is trapped by the attractor. See text for details.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0325fig2.eps} \end{figure}$	Figure 2: The topology of the freeze in ionization rotating-CAK model ( ${\delta =0}$ ), p versus $(r/R_{\ast }-1)$ for $\Omega =0.25$ . The unique curve that starts at the stellar surface and reaches infinity is the CAK original solution (continuous-line).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0325fig3.eps}\par \end{figure}$	Figure 3: The velocity profile v(r) (in km s^-1) as function of $r/R_{\ast }-1$ for the non rotating case (continuous-line) and for the rotational cases: $\Omega =0.25$ dashed-line; $\Omega =0.8$ dotted-line. The location of the singular points is indicated by a larger-dot.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{0325fig4.eps} \end{figure}$	Figure 4: Same as Figs. 1a and b but for $\delta =0.02$ . See text for discussion.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0325fig5.eps} \end{figure}$	Figure 5: The velocity profile v(r) (in km s^-1) as function of $r/R_{\ast }-1$ for the non rotating case (continuous-line) and for the rotational cases: $\Omega =0.25$ dashed-line; $\Omega =0.8$ dotted-line.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0325fig6.eps} \end{figure}$	Figure 6: The curves $r_{\rm min}$ and $r_{\pm }$ are shown with continuous lines as function of $\Omega$ . These curves represent the boundaries for the type of the singular point topology. The numerical results for the location of the singular point is also shown in dashed-line. a) is for $\delta =0.02$ and b) for $\delta =0.1$ . See text for details.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{0325fig7.eps} \end{figure}$	Figure 7: The topology of the rotating-CAK model, p versus $r/R_{\ast }-1$ for $\Omega =0.25$ and $\delta =0.02$ . The unique curve that starting at the stellar surface and reaches infinity is the CAK original solution (continuous-line).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0325fig8.eps} \end{figure}$	Figure 8: The topology of the rotating-CAK model, p versus $(r/R_{\ast }-1)$ for $\Omega =0.25$ . The different curves correspond to different values of the eigenvalues. The left-most curve starts at the "normal'' critical point and is trapped by the attractor. See text for details.
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