All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0169f1.eps} \end{figure}$ Figure 1: The acceleration-speed correlation: a) 2D distribution of events in a-v space for n4vm-subset. N is the number of events in the [ $\Delta a$ ] $\times$ [ $\Delta v$ ] = [5 m s^-2] $\times$ [20 km s^-1] bins. b) The n4v3 data. c) n4v3 bin-averaged values $\overline a_{\rm m}$ versus $\overline v_3$ for $\Delta v=100$ km s^-1 bins (beyond v>1000 km s^-1, five successive bins are merged into $\Delta v=500$ km s^-1 bins). Full lines in b) and c) show the linear least square fits, whereas 99% confidence lines are drawn dashed. d) Quadratic fit for n6v3 data (bold-dotted line) compared with the linear fit (thin-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0169f2.eps} \end{figure}$ Figure 2: Slopes $k_1=10^3\gamma _1$ of the a(v) linear fits for the n4v3-subset data sorted into $\Delta \overline \phi =10^{\circ }$ bins: a) k₁ presented as a function of bin-averaged widths $\overline \phi$ ; b) k₁ shown versus bin-averaged distances $\overline R_{\rm m}$ . The power-law least squares fits are presented together with the correlation coefficients C. In the insets analogous results are presented for the $\Delta \phi =20^{\circ }$ bins using n4v3-subset (dots), n4v5-subset (crosses), and n4vm-subset (triangles).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0169f3.eps} \end{figure}$ Figure 3: The a-v correlations shown for three $R_{\rm m}$ -bins of the n4v3, $\overline \phi =60^{\circ }$ , subset: a) $5<R_{\rm m}<7$ ( $\overline R_{\rm m}=6.01$ ); b) $7<R_{\rm m}<9$ ( $\overline R_{\rm m}=7.96$ ); c) $11<R_{\rm m}<15$ ( $\overline R_{\rm m}=13.25$ ). The number of data points is indicated (N).
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In the text

$\begin{figure} \par\includegraphics[width=17.15cm,clip]{0169f4.eps} \end{figure}$ Figure 4: Summary of the a-v correlation parameters obtained for the n4v3-subset. a) Slopes $\gamma _1$ ( top) and $\gamma _2$ ( bottom) shown as a function of bin-averaged widths $\overline \phi$ for $\overline R_{\rm m}=9$ ; b) slopes $\gamma _1$ ( top) and $\gamma _2$ ( bottom) shown as a function of bin-averaged distances $\overline R_{\rm m}$ for $\overline \phi =30^{\circ }$ (circles and fit shown in gray) and $\overline \phi =60^{\circ }$ (crosses and fit shown in black). c) The corresponding x-axis intercepts v₀ presented as a function of R and compared with the empirical solar wind model by Sheeley et al. (1997) for $w_{\infty }=400$ km s^-1 (bold-gray line). In a) and b) the power-law least squares fits for $\gamma _{1,2}(\phi )$ and $\gamma _{1,2}(R)$ are shown together with the correlation coefficients C.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0169f5.eps} \end{figure}$ Figure 5: a) A sketch showing three $a= -\gamma_2 (v-v_0)\vert v-w\vert$ curves of different $\gamma _2$ and w, and the statistical outcome for a set of nine fictive-events that were traced during a limited time interval corresponding to bold segments on the a(v)-curves. The mean acceleration and velocity of a given event is marked by circle, and the velocity interval by thin horizontal line. b) Enlarged low-velocity part of the a-v graph showing n4v3-subset data (gray), where the events with $R_{\rm m}<5$ are enhanced by black dots. Two quadratic a(v)-curves are drawn provisionally to depict the border of the "void''.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0169f6.eps} \end{figure}$ Figure 6: a) The parameter $v_0\equiv v_{a=0}$ obtained from n4v3, n6v3, n4vm, and n6vm subsets presented as a function of R. The bin-averaged widths are adjusted to $\overline \phi =30^{\circ }$ and $\overline \phi =60^{\circ }$ . The outcome is compared with the empirical solar wind model by Sheeley et al. (1997) for the asymptotic speed of $w_{\infty }=400$ and 600 km s^-1 (bold-gray and bold-black curve, respectively). b) The inferred propelling force acceleration shown in the log-log graph for the v₃ (squares) and $v_{\rm m}$ (crosses) based subsets that are shown in a). The power-law fits are indicated in black and gray, respectively. The acceleration of gravity is indicated by thin-dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0169f7.eps} \end{figure}$ Figure 7: Schematic presentation showing how the a-v correlation (bold line) is shifted in the presence of a force which gives rise to the acceleration a_x. The resulting dependence (gray-dashed line) intercepts x-axis at v₀>w if a_x>0, and at v₀<w if a_x<0.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0169f8.eps} \end{figure}$ Figure 8: a) Drag accelerations estimated using $v_{\rm m}$ for n6v3-subset, shown in the a_d-v₃ space. The corresponding linear least squares fit is indicated. b) The n6v3-subset distribution of estimated drag accelerations (black) and the corresponding inferred propelling force accelerations $a_{\rm L}$ (gray). The bin width is 5 m s^-2. 23 (0.6%) events in $a_{\rm d}$ distribution and 47 (1.3%) in $a_{\rm L}$ distribution are out of the scale. In the inset the distribution of the acceleration of gravity g is shown for bins of 1 m s^-2.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{0169f9.eps} \end{figure}$ Figure 9: The slopes $k_1=10^3\gamma _1$ of the linear a-v correlations, presented as a function of radial distance: circle - n6v3-subset; triangle - Goplaswamy et al. (2001b); square - Gopalswamy et al. (2000); crosses connected by the dotted line - Vrsnak (2001a). The power-law fit to these data-points reads k₁=1.2 R^-1.5 and is drawn by the thin-black line. The gray dashed line shows the scaling k₁ = 2 R^-1.5 inferred by Vrsnak & Gopalswamy (2002). The bold-black and bold-gray lines show power-law fits from Fig. 2b and from Fig. 4b-top for $\overline \phi =60^{\circ }$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=11.25cm,clip]{0169f10.eps} \end{figure}$ Figure 10: Distribution of CME parameters in the n4v3-subset: a) initial radial distances $R_{\rm b}$ (bins $\Delta R=1$ ); b) radial distance range $\Delta R=R_{\rm e}-R_{\rm b}$ ; c) mean radial distances $R_{\rm m}=(R_{\rm e}+R_{\rm b})/2$ ; d) angular widths ${\phi }$ (bins $\Delta \phi =20^{\circ }$ ); e) mean velocities $v_{\rm m}$ (bins $\Delta v_{\rm m}=100$ km s^-1); f) mean accelerations $a_{\rm m}$ (bins $\Delta a=5$ m s^-2); in the inset the central part of the distribution is presented (bins $\Delta a=2$ m s^-2).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{0169f11.eps} \end{figure}$ Figure 11: Relation between different CME parameters in the n4v3-subset: a) $v_{\rm m}(R_{\rm m})$ - black dots and the dashed linear least squares fit represent $\phi =360^{\circ }$ events. The $\phi <360^{\circ }$ events are depicted by gray circles and full-line least squares fit. b) $v_{\rm m}(\phi )$ ; c) $R_{\rm m}(\phi )$ . In b) and c) the $\phi =360^{\circ }$ events (crosses) are excluded from the fit.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0169f12.eps} \end{figure}$ Figure 12: a) Comparison of the a(v)-trajectory of an event moving in the $w={\rm const}.$ environment (bold-dotted arrow) with the one moving in the solar wind where the density decreases and flow speed w increases (bold arrow). The initial, mean and final velocities are denoted by b, m, and e, respectively. b) The deviation X for the approximation $\gamma _2={\rm const}.$ , $w={\rm const}.$ c) The deviation X for the solar wind speed given by Eq. (3) combined with $\gamma _2=0.76$ $\times$ 10^-6R^-0.98 (black) and $\gamma _2=5.9$ $\times$ 10^-6R^-2 (gray). The successively thicker lines in b) and c) represent v₃=1000, v₃=1500, and v₃=2000 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0169f13.eps} \end{figure}$ Figure 13: The fitted $\gamma _2(R,\phi )$ surface obtained by using Eq. (13). In the inset log-scale presentation is shown.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0169f3.eps} \end{figure}$	Figure 3: The a-v correlations shown for three $R_{\rm m}$ -bins of the n4v3, $\overline \phi =60^{\circ }$ , subset: a) $5<R_{\rm m}<7$ ( $\overline R_{\rm m}=6.01$ ); b) $7<R_{\rm m}<9$ ( $\overline R_{\rm m}=7.96$ ); c) $11<R_{\rm m}<15$ ( $\overline R_{\rm m}=13.25$ ). The number of data points is indicated (N).
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{0169f7.eps} \end{figure}$	Figure 7: Schematic presentation showing how the a-v correlation (bold line) is shifted in the presence of a force which gives rise to the acceleration a_x. The resulting dependence (gray-dashed line) intercepts x-axis at v₀>w if a_x>0, and at v₀<w if a_x<0.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{0169f13.eps} \end{figure}$	Figure 13: The fitted $\gamma _2(R,\phi )$ surface obtained by using Eq. (13). In the inset log-scale presentation is shown.
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