All Figures

$\begin{figure} \par\includegraphics[width=7cm,height=4.2cm,clip]{2287fig1.eps} %\end{figure}$ Figure 1: A portion of the red spectrum of Kapteyn's Star(solid line). Certain conspicuous features have been labelled. The "free'' boundary of the shaded region is defined by the synthetic spectrum described in the text; the shaded region shows the difference between the two. The spectra are scaled so that the total fluxes in each are the same over this wavelength interval.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,height=4.2cm,clip]{2287fig2.eps} % \end{figure}$ Figure 2: The near-IR SED of Kapteyn's Star (solid line) compared with the synthetic spectrum described in the text. As in Fig. 1, the actual GAIA synthetic spectrum is not directly plotted. The dashed line represents a NextGen synthetic spectrum corresponding to $T_{\rm eff}=3550$ K, and $[{\rm M/H}]=-0.90$ ; the superiority of the new models is apparent. The SEDs have been adjusted so that they have the same flux density at K.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig3.eps} \end{figure}$ Figure 3: The rotation curve of the model galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig4.eps} \end{figure}$ Figure 4: The KS orbit in the meridional coordinate system with no perturbation.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig5.eps} \end{figure}$ Figure 5: The Poincaré surface of the section of the orbit in Fig. 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig6.eps} \end{figure}$ Figure 6: Same orbit as Fig. 4, but with a 1% perturbation applied to the non-perturbed z-velocity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig7.eps} \end{figure}$ Figure 7: The Poincaré surface of the section of the orbit in Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig8.eps} \end{figure}$ Figure 8: Same orbit as Fig. 4, but with a 0.50% perturbation applied to the non-perturbed R-velocity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig9.eps} \end{figure}$ Figure 9: The Poincaré surface of the section of the orbit in Fig. 8.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,height=4.2cm,clip]{2287fig1.eps} %\end{figure}$	Figure 1: A portion of the red spectrum of Kapteyn's Star(solid line). Certain conspicuous features have been labelled. The "free'' boundary of the shaded region is defined by the synthetic spectrum described in the text; the shaded region shows the difference between the two. The spectra are scaled so that the total fluxes in each are the same over this wavelength interval.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig3.eps} \end{figure}$	Figure 3: The rotation curve of the model galaxy.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig4.eps} \end{figure}$	Figure 4: The KS orbit in the meridional coordinate system with no perturbation.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig5.eps} \end{figure}$	Figure 5: The Poincaré surface of the section of the orbit in Fig. 4.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig6.eps} \end{figure}$	Figure 6: Same orbit as Fig. 4, but with a 1% perturbation applied to the non-perturbed z-velocity.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig7.eps} \end{figure}$	Figure 7: The Poincaré surface of the section of the orbit in Fig. 6.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig8.eps} \end{figure}$	Figure 8: Same orbit as Fig. 4, but with a 0.50% perturbation applied to the non-perturbed R-velocity.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2287fig9.eps} \end{figure}$	Figure 9: The Poincaré surface of the section of the orbit in Fig. 8.
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