All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0060.f1.eps} \end{figure}$ Figure 1: Measured values of: a) frequency drift and b) relative band-split, presented as a function of the (fundamental) frequency at LFB, $f_{\rm L}$ . The x-axis scale is reversed accounting for the decrease of f with the radial distance. The power-law least squares fits and the corresponding correlation coefficients, C, are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0060.f2.eps} \end{figure}$ Figure 2: Inferred radial velocities versus heliocentric distances obtained using H-model: a) Complete data set; b) Bin averaged values $\overline v^*(\overline R)$ with standard deviation error bars. The empirical solar wind speed model by Sheeley et al. (1997) is shown by the thick-gray line. The thick-black line in a) represents the smoothed $\overline v^*(\overline R)$ data from b).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0060.f3.eps} \end{figure}$ Figure 3: Bin-averaged results for $\beta =0$ , $\beta =1$ , and $\beta =2$ (circles, squares, and crosses, respectively) with $w_{\infty }=400$ km s^-1. a) Magnetic field obtained utilizing H-model. The gray-full and gray-dashed lines show the power-law fits through the $\beta =0$ and $\beta =2$ DH-km data ( B=1.95 R^-1.97 and B=1.22 R^-1.97, respectively). The results based on 2S/L-model for $\beta =1$ are shown in the inset; gray line represents the function $B=2\times R^{-2}$ . b) Alfvén speed based on H-model; gray line in the IP range represents the curve $v_{\rm A}=7000 R^{-1}$ . In the inset the 2S/L model results are shown for $\beta =1$ . c) Magnetosonic speed for H-model. In the inset the H-model results for $\beta =1$ are repeated, showing the standard deviation error bars.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0060.f4.eps} \end{figure}$ Figure 4: Magnetosonic speeds inferred from the m and DH type II burst measurements by applying H-model (circles - m-range, crosses - DH-range). The 4th degree polynomial least squares fit is drawn (bold) together with the 99% confidence limits (thin). In the inset the same data are shown with two lines drawn provisionally to guide the eye.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0060.f5.eps} \end{figure}$ Figure 5: B(R) dependence beyond R=2 based on: a) Mann et al. (2003) density model; b) H-model. Circles show results for $\beta =0$ and crosses for $\beta =2$ . The gray-bold line represents $B\propto R^{-2}$ , whereas full and dashed black curves represent the equatorial dipole-current-sheet field and dipole-quadrupole-current-sheet field, after the model by Banaszkiewicz et al. (1998). The field strength is normalized to 4 nT at 1 a.u., and we take a=1.538 and K=1 (for details see Appendix B). In the insets the dependencies $v_{\rm ms}(R)$ are shown. c) Comparison of H-model density (gray-bold line) with the models by Mann et al. (2003), Withbroe (1988), and four-fold Newkirk (1967) model (full (M6), long-dashed (W), and dotted (4N) black lines, respectively).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0060.f6.eps} \end{figure}$ Figure 6: B(R) relationship obtained using H-model with $\beta =1$ and $w_\infty = 300$ , 400, and 500 km s^-1 (triangles, squares, and pluses, respectively). The power-law function is fitted only to UC/IP-range data. The coronal data are depicted by crosses.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{0060.f7.eps} \end{figure}$ Figure A.1: Density models from the AR-corona to IP space: H - the density model defined by Eq. (3); L - the L-model (Leblanc et al. 1998); 2S and 5S - two-fold and five-fold Saito (1970) model; RAE-71 - Fainberg & Stone (1971); Boug-84 - the results by Bougeret et al. (1984b) as given in Bougeret et al. (1984a); Helios - in situ measurements (Bougeret et al. 1984a); F&J-02 - Frazin & Janzen (2002).

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0060.f8.eps} \end{figure}$ Figure B.1: a) Radial dependence of the magnetic field strength B(R) in the DQCS model by Banaszkiewicz et al. (1998) in heliocentric latitude directions $b=0^{\circ }$ , $b=15^{\circ }$ , and $b=30^{\circ }$ . The case Q=0 means that there is no quadrupolar field component, whereas Q=1.5 represent the limiting case after which some field lines become detached from the photosphere (for details see Banaszkiewicz et al. 1998). Bold-dotted line represents the $B\propto R^{-2}$ dependence. b) Deviation, $\Delta b$ , of the field from radial direction. c) The ratio of the radial magnetic field components in purely radial (B_r) and DQCS-model (B^*_r) field case.

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0060.f1.eps} \end{figure}$	Figure 1: Measured values of: a) frequency drift and b) relative band-split, presented as a function of the (fundamental) frequency at LFB, $f_{\rm L}$ . The x-axis scale is reversed accounting for the decrease of f with the radial distance. The power-law least squares fits and the corresponding correlation coefficients, C, are shown.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0060.f2.eps} \end{figure}$	Figure 2: Inferred radial velocities versus heliocentric distances obtained using H-model: a) Complete data set; b) Bin averaged values $\overline v^(\overline R)$ with standard deviation error bars. The empirical solar wind speed model by Sheeley et al. (1997) is shown by the thick-gray line. The thick-black line in a) represents the smoothed $\overline v^(\overline R)$ data from b).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0060.f4.eps} \end{figure}$	Figure 4: Magnetosonic speeds inferred from the m and DH type II burst measurements by applying H-model (circles - m-range, crosses - DH-range). The 4th degree polynomial least squares fit is drawn (bold) together with the 99% confidence limits (thin). In the inset the same data are shown with two lines drawn provisionally to guide the eye.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0060.f6.eps} \end{figure}$	Figure 6: B(R) relationship obtained using H-model with $\beta =1$ and $w_\infty = 300$ , 400, and 500 km s^-1 (triangles, squares, and pluses, respectively). The power-law function is fitted only to UC/IP-range data. The coronal data are depicted by crosses.
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