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$\begin{figure} \par\includegraphics[width=16.2cm,clip]{4624fig1.eps} \end{figure}$ Figure 1: a) The poloidal magnetic field configuration given as contours of the magnetic flux function. The equator points upward. The line of force on which the model equations are solved is displayed by the thick contour. This field line is located at $\theta =70^\circ$ at 1 AU and originates from $31.5^\circ$ on the Sun. b) Radial distribution of the poloidal magnetic field strength B_l along the designated field line. At 1 AU, B_l is $3.3\gamma$ .
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{4624fig2.eps} \end{figure}$ Figure 2: Results derived from a 1.5D 3-fluid solar wind model which incorporates the azimuthal components self-consistently. The radial distribution of a) the densities of protons $n_{\rm p}$ and alpha particles $n_\alpha$ (solid lines), as well as electrons $n_{\rm e}$ (dashed line), b) the poloidal flow speeds of protons ( $v_{{\rm p}l}$ ) and alphas ( $v_{\alpha l}$ ), and c) the temperatures of electrons ( $T_{\rm e}$ ), protons ( $T_{\rm p}$ ) and alpha particles ( $T_\alpha$ ). The error bars in a) are the upper and lower limits for the electron density derived by Fisher & Guhathakurta (1995). The error bars in c) represent the uncertainties of UVCS measurements for the effective proton temperature reported by Kohl et al. (1998). Please note that both measurements are made for polar coronal holes.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4624fig3.eps} \end{figure}$ Figure 3: Radial distributions of a) the differential streaming, $v_{\alpha l}-v_{{\rm p} l}$ , and b) the poloidal flow speeds of protons ( $v_{{\rm p}l}$ ) and alpha particles ( $v_{\alpha l}$ ). Solid lines are used to plot the 1.5D model, whereas dotted lines are used for the corresponding 1D model which neglects the solar rotation.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{4624fig4.eps} \end{figure}$ Figure 4: Radial distributions of a) $-\tan\Phi=-B_\phi/B_l$ where $\Phi$ is the magnetic azimuthal angle, b) the azimuthal speeds of protons ${v}_{{\rm p} \phi }$ , alpha particles ${v}_{\alpha \phi }$ as well as electrons $v_{\rm e\phi }$ , c) the relative importance of the proton fluid $\xi _{\rm p} = {\cal L}_{\rm p}/{\cal L}$ , the alpha fluid $\xi _\alpha = {\cal L}_\alpha /{\cal L}$ , the sum of the two $\xi _{\rm P} = \xi _{\rm p}+\xi _\alpha$ , and the magnetic stresses $\xi _{\rm M} = {\cal L}_{\rm M}/{\cal L}$ in the total angular momentum loss of the Sun (please see Eq. (16) in text). In addition, the ratio of the Poynting flux to the total energy flux, $\zeta$ , is plotted as dotted line. The dashed line represents negative values. In panel b), the asterisks denote the Alfvénic point, where the poloidal Alfvénic Mach number (defined by Eq. (20)) equals unity.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4624fig3.eps} \end{figure}$	Figure 3: Radial distributions of a) the differential streaming, $v_{\alpha l}-v_{{\rm p} l}$ , and b) the poloidal flow speeds of protons ( $v_{{\rm p}l}$ ) and alpha particles ( $v_{\alpha l}$ ). Solid lines are used to plot the 1.5D model, whereas dotted lines are used for the corresponding 1D model which neglects the solar rotation.
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