All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig1.eps} \end{figure}$ Figure 1: Overview of the Moreton and EIT waves of E1 to E12. The visually determined H $\alpha$ (black) and EIT wavefronts (white) are plotted on H $\alpha$ images from the time of the wave onset (for E9, the He I fronts are shown instead of EIT). Also shown are parts of great circles which define the sectors in which the distances of the wavefronts from the calculated starting point were measured (for the cases where H $\alpha$ and EIT waves were measured using different sectors, both of them are shown). In this and all subsequent images, solar north is up, west is right, and times are given in UT.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig2.eps} \end{figure}$ Figure 2: Evolution of the flare wave of 1998 May 2 (E5) as shown by H $\alpha$ a), b), d), e) and EIT c) difference images. The wavefronts are indicated by arrows.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig3.eps} \end{figure}$ Figure 3: The flare wave of 1997 November 3 (E3) as shown by H $\alpha$ a), SXT b), d) and EIT c) difference images. The black features in the SXT images are artifacts of saturation.
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{0332fig4.eps}} \end{figure}$ Figure 4: The flare wave of 1998 August 24 (E9) as shown by He I difference images a), c) and H $\alpha$ running difference images b), d). The black circle in a) and c) indicates an area of decreased He I absorption.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig5.eps} \end{figure}$ Figure 5: The flare wave of 1998 August 8 (E6) as shown by 17 GHz difference images b)- e). a) is a pre-event direct radioheliogram showing the flaring active region and the undisturbed chromosphere.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0332fig6.eps}} \end{figure}$ Figure 6: Upper part: deprojected leading edges of the first observed H $\alpha$ wavefronts ( black), shown together with a circular fit ( grey). Lower part: deprojected leading edges of the first EIT wavefronts in E1, E3, and E5, and of the first He I wavefront in E9. In all plots, solar north is up. The individual plots are not shown to scale.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig7.eps} \end{figure}$ Figure 7: The kinematics of the leading edges of the Moreton waves (visually determined from H $\alpha$ difference images) of the events E1 to E12 (excluding E3, where only one wavefront was observed). The distances r(t) ( crosses) are plotted together with 2nd degree polynomial least-squares fits (thick line) and power-law fits (thin line). The time t is counted from the estimated starting time $t_{0~{\rm est}}$ (t0 in these plots). Distances are given in Mm (10³ km).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig8.eps} \end{figure}$ Figure 8: The velocities v(t) ( crosses) derived from consecutive Moreton wavefront pairs of events E1 to E12 (excluding E3). Also shown is the derivative of the power-law fits of r(t) (thick line) and a 2nd degree polynomial fit of v(t) (thin line). Velocities are given in km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig9.eps} \end{figure}$ Figure 9: The combined kinematics of the Moreton and EIT wavefronts for all events with EIT data coverage, except for E9 where H $\alpha$ is combined with He I. $r_{\rm H\alpha }(t)$ ( crosses) and $r_{\rm EIT}(t)$ ( circles) are plotted together with 2nd degree polynomial fits (thick line) and power-law fits (thin line) of the combined distances r(t). For E3, the positions of the X-ray wave ( triangles) are indicated, too, while for E9, both $r_{\rm H\alpha }(t)$ and $r_{\rm He~{\scriptsize I}}(t)$ ( diamonds) are plotted together with 2nd degree polynomial fits of the two data types. For E12, $r_{\rm He~{\scriptsize I}}(t)$ (determined with the "profile" method) is shown together with the fits of the combined H $\alpha$ and EIT fronts.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig2.eps} \end{figure}$	Figure 2: Evolution of the flare wave of 1998 May 2 (E5) as shown by H $\alpha$ a), b), d), e) and EIT c) difference images. The wavefronts are indicated by arrows.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig3.eps} \end{figure}$	Figure 3: The flare wave of 1997 November 3 (E3) as shown by H $\alpha$ a), SXT b), d) and EIT c) difference images. The black features in the SXT images are artifacts of saturation.
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$\begin{figure} \par\resizebox{\hsize}{!}{\includegraphics[clip]{0332fig4.eps}} \end{figure}$	Figure 4: The flare wave of 1998 August 24 (E9) as shown by He I difference images a), c) and H $\alpha$ running difference images b), d). The black circle in a) and c) indicates an area of decreased He I absorption.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig5.eps} \end{figure}$	Figure 5: The flare wave of 1998 August 8 (E6) as shown by 17 GHz difference images b)- e). a) is a pre-event direct radioheliogram showing the flaring active region and the undisturbed chromosphere.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics[clip]{0332fig6.eps}} \end{figure}$	Figure 6: Upper part: deprojected leading edges of the first observed H $\alpha$ wavefronts ( black), shown together with a circular fit ( grey). Lower part: deprojected leading edges of the first EIT wavefronts in E1, E3, and E5, and of the first He I wavefront in E9. In all plots, solar north is up. The individual plots are not shown to scale.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{0332fig8.eps} \end{figure}$	Figure 8: The velocities v(t) ( crosses) derived from consecutive Moreton wavefront pairs of events E1 to E12 (excluding E3). Also shown is the derivative of the power-law fits of r(t) (thick line) and a 2nd degree polynomial fit of v(t) (thin line). Velocities are given in km s^-1.
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