All Figures

$\begin{figure} \par\includegraphics[width=14.5cm,clip]{3109fig1.eps} \end{figure}$ Figure 1: The distribution of various parameters with time. In the cases where more than HCME could be connected with the shock at L1, the likely HCME is indicated with a black circle, while the others are the white circles. In panels a) (shock speed $V_{\rm S}$ ), b) (average transient speed $V_{\rm AVE}$ ) and c) (projected speed as measured by LASCO $V_{\rm PROJ}$ ), the average solar wind (417 km s^-1) is indicated by the solid horizontal line, while the first standard deviation ( $\pm$ 88 km s^-1) shown as the dashed lines. d) Acceleration. The dashed line indicates 0 m/s². e) Increase in B field $\Delta B_{\rm IMF}$ and f) increase in density $\Delta N$ across the shock. g) Estimated HCME width. The solid lines indicate 45 $^\circ$ , 90 $^\circ$ and 135 $^\circ$ . h) Flare class $I_{\rm FLARE}$ on a log-linear plot. Solid lines indicate the limits of each class.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3109fig2.eps} \end{figure}$ Figure 2: Variation of a) average transient speed and b) LASCO speed with acceleration. In both cases the zero acceleration line and the average solar wind speed and first standard deviation are shown. In panel a) the 2nd-order polynomial fit for $a = -2V_{\rm SW}^2/D$ , where $V_{\rm SW}$ is the average solar wind speed is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3109fig3.eps} \end{figure}$ Figure 3: Change in IMF vs. a) shock speed, b) average transient speed, c) projected LASCO speed and d) change in density. In all four cases the linear least squares fit is shown. The equations of each are a) $\Delta B_{\rm IMF} = 1.7\times 10^{-2}\Delta V + 3.6$ (R² = 0.6), b) $\Delta B_{\rm IMF} = 9.0\times 10^{-4}\Delta V + 5.9$ (R² = 0.2), c) $\Delta B_{\rm IMF} = 1.1\times 10^{-2}\Delta V + 5.1$ (R² = 0.1) and d) $\Delta B_{\rm IMF} = 2.0\times 10^{-1}\Delta N + 4.3$ (R² = 0.5). In panel a) the other dashed line is the limit of the apparent "void'' in the data, with equation $\Delta B_{\rm IMF} = 10\Delta V$ and the average and standard deviation of the solar wind speed are shown in panel c).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3109fig4.eps} \end{figure}$ Figure 4: Plot of shock speed vs. LASCO speed, both given as unitless quantities relative to the solar wind speed (i.e. $V_{\rm S}$ / $V_{\rm SW}$ vs. $V_{\rm PROJ}/V_{\rm SW}$ ) for each event. The vertical and horizontal dashed lines represent where $V_{\rm S}$ and $V_{\rm LASCO} = V_{\rm SW}$ respectively, and the $V_{\rm S} = V_{\rm PROJ}$ line of gradient = 1 is also shown as a dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3109fig5.eps} \end{figure}$ Figure 5: Flare class (intensity) plotted against LASCO speed. The solid horizontal lines indicated the limits of each class of flare are shown. Vertical lines indicate the average (and standard deviation) solar wind speed(s) while the three remaining dashed lines represent the upper and lower "voids'' of points, spanning the regions $\log I_{\rm FLARE} > 26.3 V_{\rm PROJ} + 300$ and $\log I_{\rm FLARE} < 1.3 V_{\rm PROJ} - 1610$ , and the linear least squares fit, of equation $\log I_{\rm FLARE} = 2.0V_{\rm PROJ} - 1.1\times 10^3$ (R² = 0.4).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{3109fig6.eps} \end{figure}$ Figure 6: a) and c) $A_{\rm p}$ and b) and d) Dst vs. a) and b) projected LASCO speed and c) and d) shock speed for the events associated with a geomagnetic storm. In all cases the average and first standard deviation from the average solar wind speed is given, and also the linear least squares fit for each case. The equations of these are: a) $A_{\rm p} = 2.5\times 10^{-2} V_{\rm PROJ} + 48.4$ ( R² = 0.21), b) Dst $= -5.9\times 10^{-2} V_{\rm PROJ} - 96.3$ (R² = 0.17) c) $A_{\rm p} = 7.3\times 10^{-2} V_{\rm S} + 19.2$ ( R² = 0.34) and d) Dst $= -1.7\times 10^{-1} V_{\rm S} - 41.8$ ( R² = 0.23).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3109fig7.eps} \end{figure}$ Figure 7: Flare class vs. a) $A_{\rm p}$ and b) Dst for the events associated with the storms. In both cases the limits of each flare class is indicated by the solid lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3109fig2.eps} \end{figure}$	Figure 2: Variation of a) average transient speed and b) LASCO speed with acceleration. In both cases the zero acceleration line and the average solar wind speed and first standard deviation are shown. In panel a) the 2nd-order polynomial fit for $a = -2V_{\rm SW}^2/D$ , where $V_{\rm SW}$ is the average solar wind speed is indicated.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3109fig7.eps} \end{figure}$	Figure 7: Flare class vs. a) $A_{\rm p}$ and b) Dst for the events associated with the storms. In both cases the limits of each flare class is indicated by the solid lines.
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