$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0538fig1.eps} \end{figure}$ Figure 1: Self-similar solutions corresponding to $\gamma =4/3$ , $\eta _{0}=0.1$ and $\beta _0=0.1$ . Top: magnetic flux function $\phi (\theta )$ as a function of polar angle $\theta$ . Middle: Radial velocity $V(\theta )$ . Bottom: density $R(\theta )$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0538fig3.eps} \end{figure}$ Figure 3: Representation of magnetic field lines in the meridional plane for a typical self-similar solution with $\eta _{0}=0.1$ , $\gamma =4/3$ and f=0.84.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0538fig4.eps} \end{figure}$ Figure 4: The net accretion rate $\dot{M}/\dot{M}_{\rm Bondi}$ as a function of the advected energy f for the self-similar solutions shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0538fig1.eps} \end{figure}$	Figure 1: Self-similar solutions corresponding to $\gamma =4/3$ , $\eta _{0}=0.1$ and $\beta _0=0.1$ . Top: magnetic flux function $\phi (\theta )$ as a function of polar angle $\theta$ . Middle: Radial velocity $V(\theta )$ . Bottom: density $R(\theta )$ .
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0538fig2.eps} \end{figure}$	Figure 2: Ratio of the thermal to the magnetic pressures for the solutions shown in Fig. 1.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0538fig3.eps} \end{figure}$	Figure 3: Representation of magnetic field lines in the meridional plane for a typical self-similar solution with $\eta _{0}=0.1$ , $\gamma =4/3$ and f=0.84.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{0538fig4.eps} \end{figure}$	Figure 4: The net accretion rate $\dot{M}/\dot{M}_{\rm Bondi}$ as a function of the advected energy f for the self-similar solutions shown in Fig. 1.
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