All Figures

$\begin{figure} \par\mbox{\subfigure[2000QC$_{243}$ ]{\includegraphics[width=7.2c... ...{255}$ ]{\includegraphics[width=7.2cm,height=9.9cm]{H4130F1b.ps} }} \end{figure}$ Figure 1: Numerically integrated orbital elements of a) 2000QC₂₄₃ and b) 2001XZ₂₅₅. The bottom panels show the critical arguments: $\sigma = 5 \lambda _{\rm U} - 4 \lambda - \varpi$ for 2000QC₂₄₃and $\sigma = 4 \lambda _{\rm U} - 3 \lambda - \varpi$ for 2001XZ₂₅₅. They librate around 0 degrees.
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In the text

$\begin{figure} \par\mbox{\subfigure[2000QC$_{243}$ ]{\includegraphics[width=5.8c... ...55}$ ]{\includegraphics[width=5.8cm,height=4.35cm]{H4130F2b.eps} }} \end{figure}$ Figure 2: Orbital evolution on an (a, e) plane. The plotted data cover from -1 Myr to +1 Myr. For convenience, the planet-crossing curves are also shown. For drawing these curves, we assume that the Centaur and giant planets are moving on a common plane and the planetary eccentricities are fixed to the present values.
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In the text

$\begin{figure} \par\mbox{\subfigure[(10199) Chariklo]{\includegraphics[width=7.1... ...0~kyr)]{\includegraphics[width=7.1cm,height=9.76cm]{H4130F3b.ps} }} \end{figure}$ Figure 3: Numerically integrated orbital elements of a) (10199) Chariklo and b) 1994TA (-30 kyr to + 30 kyr). The bottom panels show the critical arguments of $\sigma = 4 \lambda _{\rm U} - 3 \lambda - \varpi$ for (10199) Chariklo and $\sigma = 11 \lambda _{\rm U} - 9 \lambda - 2 \varpi _{\rm U}$ for 1994TA. (10199) Chariklo is not in the resonance at present.
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In the text

$\begin{figure} \par\subfigure[2000QC$_{243}$ ]{\includegraphics[width=10.7cm,hei... ...55}$ ]{\includegraphics[width=10.7cm,height=7.13cm]{H4130F4b.eps} } \end{figure}$ Figure 4: Clone tests for a) 2000QC₂₄₃ and b) 2001XZ₂₅₅. Each panel corresponds to one clone particle. The initial orbital elements are shifted by small amounts designated as $\Delta a$ AU and $\Delta e$ at the top and the left of the figures. The time-evolution of the critical argument is plotted on a $(t, \sigma )$ plane; the horizontal axis spans from 0 to 50 000 years (one division equals 10 000 years) and the vertical axis spans from -180 to 180 degrees (one division equals 90 degrees). The result of the original orbital data listed in Table 1 is plotted on a panel with a thick frame which is located at $\Delta a = 0.00$ AU and $\Delta e = 0.00$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm,height=6.2cm,clip]{H4130F5.eps}\end{figure}$ Figure 5: Orbital evolution of other Centaurs near the resonant candidates. We plot the evolutional tracks on an (a, e) plane for the next 50 000 years. These objects are not wandering around so much on the (a, e) plane, in contrast to other Centaurs which have eccentric and/or planet-crossing orbits. Large orbital changes in the elements of 1994TA occur after the resonance is unlocked. The present orbital inclinations (unit: degree) are also indicated in parentheses.
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In the text

$\begin{figure} \par\mbox{\subfigure[2000QC$_{243}$ ]{\includegraphics[width=7.2c... ...{255}$ ]{\includegraphics[width=7.2cm,height=9.9cm]{H4130F1b.ps} }} \end{figure}$	Figure 1: Numerically integrated orbital elements of a) 2000QC₂₄₃ and b) 2001XZ₂₅₅. The bottom panels show the critical arguments: $\sigma = 5 \lambda _{\rm U} - 4 \lambda - \varpi$ for 2000QC₂₄₃and $\sigma = 4 \lambda _{\rm U} - 3 \lambda - \varpi$ for 2001XZ₂₅₅. They librate around 0 degrees.
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$\begin{figure} \par\mbox{\subfigure[2000QC$_{243}$ ]{\includegraphics[width=5.8c... ...55}$ ]{\includegraphics[width=5.8cm,height=4.35cm]{H4130F2b.eps} }} \end{figure}$	Figure 2: Orbital evolution on an (a, e) plane. The plotted data cover from -1 Myr to +1 Myr. For convenience, the planet-crossing curves are also shown. For drawing these curves, we assume that the Centaur and giant planets are moving on a common plane and the planetary eccentricities are fixed to the present values.
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$\begin{figure} \par\mbox{\subfigure[(10199) Chariklo]{\includegraphics[width=7.1... ...0~kyr)]{\includegraphics[width=7.1cm,height=9.76cm]{H4130F3b.ps} }} \end{figure}$	Figure 3: Numerically integrated orbital elements of a) (10199) Chariklo and b) 1994TA (-30 kyr to + 30 kyr). The bottom panels show the critical arguments of $\sigma = 4 \lambda _{\rm U} - 3 \lambda - \varpi$ for (10199) Chariklo and $\sigma = 11 \lambda _{\rm U} - 9 \lambda - 2 \varpi _{\rm U}$ for 1994TA. (10199) Chariklo is not in the resonance at present.
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