All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6284f1.ps}\end{figure}$ Figure 1: Stability of the Lagrange point L₄ taking the outer planet's perturbations into account. On the x-axis we plotted the initial semimajor axes, on the y-axis the initial eccentricity of the second planet; light grey indicates unstable motions, and dark grey indicates motion of a stable Trojan, where we used $e_{\rm max}$ during the whole integration as a check.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6284f2.ps}\end{figure}$ Figure 2: Captions similar to Fig.1 but with results from the computations of the FLIs. GG2 stands for the outer Gasgiant.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6284f3.ps}\end{figure}$ Figure 3: FLI for different initial conditions of the outer planet in a (x-axis) and e (y-axis). In the upper left corner the two giant planets are in a weak chaotic zone, and the large region in dark grey corresponds to regular orbits of both planets.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{6284f4.ps}\end{figure}$ Figure 4: The chaotic orbits of both planets of HD 108874 with the initial conditions M13 for 10⁸ years.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f5.ps}\par\vspace*{1.2cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f6.ps}\end{figure}$ Figure 5: Stability regions around L₄ in Models M21 and M22. The initial semimajor axis (y-axis) is plotted versus the initial angular distance from the equilibrium point L₄. The dark regions around the point L₄ (a=1.051 AU, $\omega =308$ ) show that the maximum eccentricity during the integration time was always $e_{\max} < 0.3$ with such initial conditions.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f7.ps}\par\vspace*{1.2cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f8.ps}\end{figure}$ Figure 6: Captions like in Fig. 4 but for the models M31 and M32.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=6.7cm,clip]{6284f9.ps}\end{figure}$ Figure 7: Cuts with a fixed semimajor axis with changing angular distance to the Lagrange point L₄, which is located at $\omega = 308^{\circ }$ . The different curves show how the extension of the stable region shrinks with the integration time; full line results after 10⁷ years, dotted line after 10⁶ years, hatched region after 10⁵ years.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f10.ps}\par\vspace*{0.8cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f11.ps}\end{figure}$ Figure 8: Cut with a fixed semimajor axis and cut with a fixed pericenter; upper graph for model M21, lower graph for model M22. The crossing of the two lines is the Lagrange point L₄; the z-axis is the maximum eccentricity for the integration time of 10⁷ years.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.9cm,clip]{6284f12.ps}\end{figure}$ Figure 9: Cut with a fixed semimajor axis and cut with a fixed pericenter for the model M31^*. This model presents the results for more massive planets (50 percent larger) to take into account the influence of the inclination of the orbits with respect to the line of sight of the observations. The crossing of the two lines is the Lagrange point L₄; the z-axis is the maximum eccentricity.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6284f1.ps}\end{figure}$	Figure 1: Stability of the Lagrange point L₄ taking the outer planet's perturbations into account. On the x-axis we plotted the initial semimajor axes, on the y-axis the initial eccentricity of the second planet; light grey indicates unstable motions, and dark grey indicates motion of a stable Trojan, where we used $e_{\rm max}$ during the whole integration as a check.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6284f2.ps}\end{figure}$	Figure 2: Captions similar to Fig.1 but with results from the computations of the FLIs. GG2 stands for the outer Gasgiant.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6284f3.ps}\end{figure}$	Figure 3: FLI for different initial conditions of the outer planet in a (x-axis) and e (y-axis). In the upper left corner the two giant planets are in a weak chaotic zone, and the large region in dark grey corresponds to regular orbits of both planets.
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$\begin{figure} \par\includegraphics[angle=270,width=6.9cm,clip]{6284f4.ps}\end{figure}$	Figure 4: The chaotic orbits of both planets of HD 108874 with the initial conditions M13 for 10⁸ years.
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$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f5.ps}\par\vspace*{1.2cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f6.ps}\end{figure}$	Figure 5: Stability regions around L₄ in Models M21 and M22. The initial semimajor axis (y-axis) is plotted versus the initial angular distance from the equilibrium point L₄. The dark regions around the point L₄ (a=1.051 AU, $\omega =308$ ) show that the maximum eccentricity during the integration time was always $e_{\max} < 0.3$ with such initial conditions.
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$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f7.ps}\par\vspace*{1.2cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f8.ps}\end{figure}$	Figure 6: Captions like in Fig. 4 but for the models M31 and M32.
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$\begin{figure} \par\includegraphics[angle=270,width=6.7cm,clip]{6284f9.ps}\end{figure}$	Figure 7: Cuts with a fixed semimajor axis with changing angular distance to the Lagrange point L₄, which is located at $\omega = 308^{\circ }$ . The different curves show how the extension of the stable region shrinks with the integration time; full line results after 10⁷ years, dotted line after 10⁶ years, hatched region after 10⁵ years.
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$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{6284f10.ps}\par\vspace*{0.8cm} \includegraphics[angle=270,width=7.4cm,clip]{6284f11.ps}\end{figure}$	Figure 8: Cut with a fixed semimajor axis and cut with a fixed pericenter; upper graph for model M21, lower graph for model M22. The crossing of the two lines is the Lagrange point L₄; the z-axis is the maximum eccentricity for the integration time of 10⁷ years.
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$\begin{figure} \par\includegraphics[angle=270,width=7.9cm,clip]{6284f12.ps}\end{figure}$	Figure 9: Cut with a fixed semimajor axis and cut with a fixed pericenter for the model M31^*. This model presents the results for more massive planets (50 percent larger) to take into account the influence of the inclination of the orbits with respect to the line of sight of the observations. The crossing of the two lines is the Lagrange point L₄; the z-axis is the maximum eccentricity.
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