All Figures

$\begin{figure} \par\includegraphics[width=16cm,clip]{4282fig1}\end{figure}$ Figure 1: Butterfly diagram from 1874 to 2005 based on data from the Royal Greenwich Observatory up to 1976, from the former Soviet Union between 1977 and 1985 and from the Mount Wilson Solar Observatory from 1986 onward. The vertical dashed lines mark the official minima of the sunspot cycle, the inclined solid lines our estimates of the boundaries between individual cycles. Cycle numbers are marked at the top of each cycle.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4282fig2}}\end{figure}$ Figure 2: Two examples of the latitude distribution of the cycle-integrated sunspot area. a) cycle 12, b) cycle 19 (dots). The solid lines represent 5 $^\circ$ running means.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{4282fig3}\end{figure}$ Figure 3: Relationships between parameters describing the latitude dependence of the sunspot distribution. In the three columns we plot results obtained for the northern hemisphere (left), the southern hemisphere (middle) and the parameters averaged over both hemispheres (right). From top to bottom we plot $\langle l \rangle$ vs. $A_{\rm tot}$ , $\sigma$ vs. $A_{\rm tot}$ , $\sigma$ vs. $\langle l \rangle$ , s vs. $\sigma$ and k vs. s. Open circles: cycle 12, filled circles: 13, open triangles: 14, filled triangles: 15, open squares: 16, filled squares: 17, open diamonds: 18, filled diamonds: 19, pluses: 20, crosses: 21, crossed squares: 22. The solid lines are least squares fits. The dashed lines represent fits to cycles 12-20 alone (RGO data).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4282fig4}\end{figure}$ Figure 4: Difference between correlation coefficients $r_{\rm c}$ between ``moments'' of latitude distributions of sunspots in the northern, $r_{\rm c}(N)$ and the southern hemispheres, $r_{\rm c}(S)$ vs. $r_{\rm c}(\langle N+S \rangle)$ (top panel). In the middle and bottom panels the difference between $r_{\rm c}(\langle N+S \rangle)$ , and $r_{\rm c}(N)$ or $r_{\rm c}(S)$ , respectively, are plotted. Open circles: $\langle l \rangle$ vs. $A_{\rm tot}$ , filled circles: $\sigma$ vs. $A_{\rm tot}$ , open triangles: s vs. $A_{\rm tot}$ , filled triangles: k vs. $A_{\rm tot}$ , open squares: $\sigma$ vs. $\langle l \rangle$ , filled squares: s vs. $\langle l \rangle$ , open diamonds: k vs. $\langle l \rangle$ , filled diamonds: s vs. $\sigma$ , pluses: k vs. $\sigma$ , crosses: k vs. s.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4282fig5}}\end{figure}$ Figure 5: Latitude distributions of the cycle-integrated sunspot area. $5^\circ$ running means are plotted. Colour key is given at the top of the plot. The thick black line represents the mean cycle distribution.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17cm,clip]{4282fig6}\end{figure}$ Figure 6: Butterfly diagrams for the northern hemisphere produced by 5 simple dynamo models described in the text. Shown are contours of field strength, with negative fields being indicated by dashed contours. Time is measured in units of diffusion time.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{4282fig7}\end{figure}$ Figure 7: Latitude distribution of cycle-averaged magnetic flux above the threshold for each of the 5 considered dynamo models. Plotted is the distribution averaged over all cycles (thick curves), as well as the distributions due to the strongest and weakest analysed cycles.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{4282fig8}\end{figure}$ Figure 8: Difference between correlation coefficients $r_{\rm c}$ obtained from solar data and from models, plotted vs. the observed $r_{\rm c}$ . The three frames refer from left to right to solar $r_{\rm c}$ values deduced from the northern hemisphere, the southern hemisphere and the whole Sun. From top to bottom the frames refer to models A to E. Open circles: $\langle l \rangle$ vs. $A_{\rm tot}$ , filled circles: $\sigma$ vs. $A_{\rm tot}$ , open triangles: s vs. $A_{\rm tot}$ , filled triangles: k vs. $A_{\rm tot}$ , open squares: $\sigma$ vs. $\langle l \rangle$ , filled squares: s vs. $\langle l \rangle$ , open diamonds: k vs. $\langle l \rangle$ , filled diamonds: s vs. $\sigma$ , pluses: k vs. $\sigma$ , crosses: k vs. s.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4282fig2}}\end{figure}$	Figure 2: Two examples of the latitude distribution of the cycle-integrated sunspot area. a) cycle 12, b) cycle 19 (dots). The solid lines represent 5 $^\circ$ running means.
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$\begin{figure} \resizebox{8.8cm}{!}{\includegraphics{4282fig5}}\end{figure}$	Figure 5: Latitude distributions of the cycle-integrated sunspot area. $5^\circ$ running means are plotted. Colour key is given at the top of the plot. The thick black line represents the mean cycle distribution.
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$\begin{figure} \par\includegraphics[angle=90,width=17cm,clip]{4282fig6}\end{figure}$	Figure 6: Butterfly diagrams for the northern hemisphere produced by 5 simple dynamo models described in the text. Shown are contours of field strength, with negative fields being indicated by dashed contours. Time is measured in units of diffusion time.
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$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{4282fig7}\end{figure}$	Figure 7: Latitude distribution of cycle-averaged magnetic flux above the threshold for each of the 5 considered dynamo models. Plotted is the distribution averaged over all cycles (thick curves), as well as the distributions due to the strongest and weakest analysed cycles.
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