All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{contour_r=0.64.eps} \end{figure}$ Figure 1: Contours of the zero-order rotation profile $\Omega _0={\rm constant}$ with r₀=0.64. The darker contours indicate slower rotation.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.2.Calpha=-1.4.a=0.1.... ...cludegraphics[width=6cm,clip]{TO-butt.r0=0.2.Calpha=-1.4.a=0.1.eps} \end{figure}$ Figure 2: The radial r-t contours of the angular velocity residuals $\delta \Omega$ as a function of time for a cut at 10 degrees latitude, as well as the corresponding butterfly diagram (i.e. latitude-time plot) for the toroidal component of the magnetic field ${\vec B}$ and the torsional oscillation butterfly diagram near the surface for a dynamo region with r₀=0.2, a=0.1 and $R_\alpha =-1.4$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and the presence of a weak polar branch.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{fragmentation.r=0.2.Calpha=-2.50.eps} \end{figure}$ Figure 3: The r-t diagram for torsional oscillations showing spatiotemporal fragmentation. Note the contrast between the top of the dynamo region and the bottom, where the period is halved.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.2.Calpha=-8.a=0.01.e... ...ncludegraphics[width=6cm,clip]{TO-butt.r0=0.2.Calpha=-8.a=0.01.eps} \end{figure}$ Figure 4: As in Fig. 2 for a dynamo region with r₀=0.2, a=0.01 and $R_\alpha =-8$ . Note the presence of torsional oscillations near both top and the bottom of the dynamo region.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{butterfly.r=0.99.Calpha=-10.... ...raphics[width=6cm,clip]{residuals.v.10.degrees.Calpha-10.r=0.2.eps} \end{figure}$ Figure 5: An example of a noisy periodic regime before the onset of fully chaotic behaviour. The top panel shows the magnetic butterfly diagram close to the surface with the usual solar-type migration towards the equator, whilst also showing slight equatorial asymmetry. The bottom panel shows the r-t diagram for the torsional oscillations, again showing the onset of break-up of periodicity.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.64.Calpha=-2.a=0.1.e... ...ncludegraphics[width=6cm,clip]{TO-butt.r0=0.64.Calpha=-2.a=0.1.eps} \end{figure}$ Figure 6: As in Fig. 2 for a dynamo region with r₀=0.64, a=0.1 and $R_\alpha =-2$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.64.Calpha=-12.a=0.01... ...ludegraphics[width=6cm,clip]{TO-butt.r0=0.64.Calpha=-12.a=0.01.eps} \end{figure}$ Figure 7: As in Fig. 2 for a dynamo region with r₀=0.64, a=0.01 and $R_\alpha =-12$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.775.Calpha=-5.a=0.1.... ...cludegraphics[width=6cm,clip]{TO-butt.r0=0.775.Calpha=-5.a=0.1.eps} \end{figure}$ Figure 8: As in Fig. 2 for a dynamo region with r₀=0.775, a=0.1 and $R_\alpha =-5$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{TO.r0=0.775.Calpha=-17.a=0... ...egraphics[width=6.2cm,clip]{TO-butt.r0=0.775.Calpha=-17.a=0.01.eps} \end{figure}$ Figure 9: As in Fig. 2 for a dynamo region with r₀=0.775, a=0.01 and $R_\alpha =-17$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{disruptionOmega.eps} \end{figure}$ Figure 10: The behaviour of $\langle\Delta\Omega\rangle$ as a function of $R_\alpha$ for models with different depths of the dynamo region.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{OmegaFullByOmegaStarAtSurfaceClean.eps} \end{figure}$ Figure 11: The fitting of our rotation profile by the parameterization (7). The model parameters used are $r_0=0.2, R_\alpha =-1.40$ and a=0.1. The continuous curve gives the values of $<\vert\Omega _t\vert>$ at the surface, whereas the crosses correspond to the interpolation $y=a_0+a_1\sin^2\theta+a_2\sin^4\theta$ - see text.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{BOXED.AVE.r=0.64.Calpha=-2.a=0.1.eps} \end{figure}$ Figure 12: The rectangular contours of the average $\Omega (r, \theta )$ normalized by $\Omega _0$ , defined by Eq. (6) for a solar-like model with r₀=0.64, $R_\alpha =-2$ and a=0.1.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{butt.r=0.64_Calph=-3.00.a=-1... ...m} \includegraphics[width=6cm,clip]{TO.r=0.64_Calph=-3.00.a=-1.eps} \end{figure}$ Figure 13: The butterfly diagrams of the near-surface magnetic field and torsional oscillations for a dynamo region with r₀=0.64, a=-0.1 and $R_\alpha =-3$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{contour_r=0.64.eps} \end{figure}$	Figure 1: Contours of the zero-order rotation profile $\Omega _0={\rm constant}$ with r₀=0.64. The darker contours indicate slower rotation.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{fragmentation.r=0.2.Calpha=-2.50.eps} \end{figure}$	Figure 3: The r-t diagram for torsional oscillations showing spatiotemporal fragmentation. Note the contrast between the top of the dynamo region and the bottom, where the period is halved.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.2.Calpha=-8.a=0.01.e... ...ncludegraphics[width=6cm,clip]{TO-butt.r0=0.2.Calpha=-8.a=0.01.eps} \end{figure}$	Figure 4: As in Fig. 2 for a dynamo region with r₀=0.2, a=0.01 and $R_\alpha =-8$ . Note the presence of torsional oscillations near both top and the bottom of the dynamo region.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{butterfly.r=0.99.Calpha=-10.... ...raphics[width=6cm,clip]{residuals.v.10.degrees.Calpha-10.r=0.2.eps} \end{figure}$	Figure 5: An example of a noisy periodic regime before the onset of fully chaotic behaviour. The top panel shows the magnetic butterfly diagram close to the surface with the usual solar-type migration towards the equator, whilst also showing slight equatorial asymmetry. The bottom panel shows the r-t diagram for the torsional oscillations, again showing the onset of break-up of periodicity.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.64.Calpha=-2.a=0.1.e... ...ncludegraphics[width=6cm,clip]{TO-butt.r0=0.64.Calpha=-2.a=0.1.eps} \end{figure}$	Figure 6: As in Fig. 2 for a dynamo region with r₀=0.64, a=0.1 and $R_\alpha =-2$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.64.Calpha=-12.a=0.01... ...ludegraphics[width=6cm,clip]{TO-butt.r0=0.64.Calpha=-12.a=0.01.eps} \end{figure}$	Figure 7: As in Fig. 2 for a dynamo region with r₀=0.64, a=0.01 and $R_\alpha =-12$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{TO.r0=0.775.Calpha=-5.a=0.1.... ...cludegraphics[width=6cm,clip]{TO-butt.r0=0.775.Calpha=-5.a=0.1.eps} \end{figure}$	Figure 8: As in Fig. 2 for a dynamo region with r₀=0.775, a=0.1 and $R_\alpha =-5$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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$\begin{figure} \par\includegraphics[width=6.2cm,clip]{TO.r0=0.775.Calpha=-17.a=0... ...egraphics[width=6.2cm,clip]{TO-butt.r0=0.775.Calpha=-17.a=0.01.eps} \end{figure}$	Figure 9: As in Fig. 2 for a dynamo region with r₀=0.775, a=0.01 and $R_\alpha =-17$ . Note the penetration of the torsional oscillations all the way down to the bottom of the dynamo region, and also the localisation of the torsional oscillations and the magnetic field near the equator.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{disruptionOmega.eps} \end{figure}$	Figure 10: The behaviour of $\langle\Delta\Omega\rangle$ as a function of $R_\alpha$ for models with different depths of the dynamo region.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{OmegaFullByOmegaStarAtSurfaceClean.eps} \end{figure}$	Figure 11: The fitting of our rotation profile by the parameterization (7). The model parameters used are $r_0=0.2, R_\alpha =-1.40$ and a=0.1. The continuous curve gives the values of $<\vert\Omega _t\vert>$ at the surface, whereas the crosses correspond to the interpolation $y=a_0+a_1\sin^2\theta+a_2\sin^4\theta$ - see text.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{BOXED.AVE.r=0.64.Calpha=-2.a=0.1.eps} \end{figure}$	Figure 12: The rectangular contours of the average $\Omega (r, \theta )$ normalized by $\Omega _0$ , defined by Eq. (6) for a solar-like model with r₀=0.64, $R_\alpha =-2$ and a=0.1.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{butt.r=0.64_Calph=-3.00.a=-1... ...m} \includegraphics[width=6cm,clip]{TO.r=0.64_Calph=-3.00.a=-1.eps} \end{figure}$	Figure 13: The butterfly diagrams of the near-surface magnetic field and torsional oscillations for a dynamo region with r₀=0.64, a=-0.1 and $R_\alpha =-3$ .
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