All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fj062_fig1.ps} \end{figure}$ Figure 1: The observed concentration of ¹⁰Be form 1500-2000. Also shown is the observed sunspot number from 1600-2000. The figure is taken from McCracken & McDonald (2001) who applied an averaging procedure to the original data published by Beer et al. (1990).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,angle=0,clip]{Fj062_fig2.ps} \end{figure}$ Figure 2: In the upper panel the solar wind speed variation for a Maunder like grand minimum is shown, see Eq. (3). In the lower panel the corresponding variation for the diffusion coefficient is shown, see Eq. (5). Note, that the increase during the simulated Maunder Minimum is not a velocity effect, but has to be attributed to a change of the solar magnetic field. The origin of time (in years) is arbitrary.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fj062_fig3.ps} \end{figure}$ Figure 3: The simulated cosmic ray variation during and around the Maunder Minimum in a dynamical heliosphere. The dashed line indicates the flux level for f₃(t)=0, see Eq. (6).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fj062_fig1.ps} \end{figure}$	Figure 1: The observed concentration of ¹⁰Be form 1500-2000. Also shown is the observed sunspot number from 1600-2000. The figure is taken from McCracken & McDonald (2001) who applied an averaging procedure to the original data published by Beer et al. (1990).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Fj062_fig3.ps} \end{figure}$	Figure 3: The simulated cosmic ray variation during and around the Maunder Minimum in a dynamical heliosphere. The dashed line indicates the flux level for f₃(t)=0, see Eq. (6).
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