All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{0992fig1.eps} \end{figure}$ Figure 1: Adopted meridional magnetic field configuration in the inner corona. Here only a quadrant is shown in which the magnetic axis points upward, and the thick contours labeled F and S delineate the lines of force along which the fast and slow solar wind solutions are examined, respectively. Also shown is how to define the geometrical factor R, and the base vectors $\hat{e}_l, \hat{e}_N$ and $\hat{e}_\phi$ of the flux tube coordinate system (see Sect. 2).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0992fig2.eps} \end{figure}$ Figure 2: Radial distribution between 1 $R_\odot$ and 1 AU of the adopted meridional flow parameters for the fast ( left column) and slow ( right) solar wind. a) and c), the meridional flow speeds of protons ( $v_{{\rm p}l}$ ) and alpha particles ( $v_{\alpha l}$ ). b) and d), the ion temperatures $T_k^{\parallel }$ (dotted lines), $T_k^{\perp }$ (dashed lines), and $T_k=(T_k^{\parallel }+2T_k^{\perp })/3$ (solid lines) where $k={\rm p}, \alpha$ . The construction of $T_k^{\parallel , \perp }$ is described in Sect. 3.2. The error bars in b) and d) represent the uncertainties of the UVCS measurements of the effective proton temperature as reported by Kohl et al. (1998) for a coronal hole, and by Frazin et al. (2003) for a streamer, respectively. Note that both measurements are typical of solar minimum conditions. Moreover, the asterisks in a) and c) denote the Alfvén point, where the meridional Alfvénic Mach number (defined by Eq. (18)) equals unity.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0992fig3.eps} \end{figure}$ Figure 3: Radial distributions of a) the proton azimuthal speed $v_{\rm p\phi }$ , b) the alpha one $v_{\alpha \phi }$ , and c) various contributions to the angular momentum budget in an $\rm e-p-\alpha$ solar wind with ion temperature anisotropies. In a) and b), the profiles derived for a solar wind with identical flow parameters where ion temperature anisotropies are neglected are given by dashed lines for comparison. Panel c) depicts the individual ion angular momentum fluxes $L_{\rm p}$ and $L_\alpha$ , their sum L_P, and the fluxes associated with the magnetic stresses $L_{\rm M}$ , and with the temperature anisotropies $L_{\rm ani}$ (see Eq. (16)). The dash-dotted lines represent negative values.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0992fig4.eps} \end{figure}$ Figure 4: Values of several parameters as a function of $\Gamma _{\rm pE}$ , the proton temperature anisotropy at 1 AU. a) The factor $\lambda$ , the deviation of which from unity represents the correction to the total angular momentum loss due to the introduction of ion pressure anisotropies; b) and c) the proton and alpha azimuthal speeds $v_{\rm p\phi }$ and $v_{\alpha \phi }$ at two different heliocentric distances given by different line styles as indicated in b); d) various components in the angular momentum flux at 1 AU including individual ion contribution $L_{\rm p}$ and $L_\alpha$ , the overall particle contribution $L_P=L_{\rm p}+L_\alpha$ , as well as the contribution from magnetic stresses $L_{\rm M}$ . Note that $-L_\alpha$ instead of $L_\alpha$ is given in d). The short horizontal bars in panels b) and c) represent the azimuthal ion speeds derived in the isotropic model for comparison. Furthermore, in panel b) the curve corresponding to 1 AU is slightly shifted relative to that for 0.3 AU to avoid the two overlapping each other. The open circles correspond to the cases where $\Gamma _{\rm\alpha E}$ is fixed at 1.3, where $\Gamma _{\rm\alpha E}$ is the alpha temperature anisotropy at 1 AU. At a given $\Gamma _{\rm pE}$ each parameter varies monotonically from the value with $\Gamma _{\rm\alpha E}=0.7$ , represented by the end of the arrow, to the value with $\Gamma _{\rm\alpha E}=1.9$ given by the arrow head. The ranges in which $\Gamma _{\rm pE}$ and $\Gamma _{\rm\alpha E}$ vary are determined from the Helios measurements (see text for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0992fig5.eps} \end{figure}$ Figure 5: Similar to Fig. 4 but for the slow solar wind. Here the open circles correspond to the cases where $\Gamma _{\rm\alpha E}$ is fixed at 1.4, and the arrow represents how the specific parameter varies at a given $\Gamma _{\rm pE}$ when $\Gamma _{\rm\alpha E}$ increases from 0.8 to 2.0.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0992fig6.eps} \end{figure}$ Figure 6: Radial dependence of the ratio of the alpha to the proton velocity fluctuation amplitudes $\delta u_\alpha /\delta u_{\rm p}$ induced by Alfvénic activities in super-Alfvénic portions of the fast solar wind. The dashed curves correspond to the isotropic model, while the hatched areas give the possible range $\delta u_\alpha /\delta u_{\rm p}$ may occupy when the parameters $\Gamma _{\rm pE}$ and $\Gamma _{\rm\alpha E}$ vary in the ranges given in text. Both the zero-frequency (upper portion) and WKB ( lower) estimates are given.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0992fig5.eps} \end{figure}$	Figure 5: Similar to Fig. 4 but for the slow solar wind. Here the open circles correspond to the cases where $\Gamma _{\rm\alpha E}$ is fixed at 1.4, and the arrow represents how the specific parameter varies at a given $\Gamma _{\rm pE}$ when $\Gamma _{\rm\alpha E}$ increases from 0.8 to 2.0.
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