All Figures

$\begin{figure} \par\mbox{\includegraphics[width=3.7cm,height=3.5cm]{09758F1a.eps... ...ce*{3mm} \includegraphics[width=3.7cm,height=3.5cm]{09758F1b.eps} } \end{figure}$ Figure 1: Setup for the circular restricted three body problem.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,height=6.5cm]{09758F2.eps}\end{figure}$ Figure 2: Locations of the Lagrange points L₁, L₂, L₃, L₄, and L₅ in synodic coordinates $X^{\ast }$ and $Y^{\ast }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F3.eps}\end{figure}$ Figure 3: For a mass ratio of $\mu = 0.5$ , runs for four different distance ratios are shown, which are ${\rho _0} = 0.200$ , 0.300, 0.425, and 0.450 (solid lines). We also show the zero velocity contours (dash-dotted lines) indicating the permitted regions of motion and the Lagrange points (crosses).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F4.eps}\end{figure}$ Figure 4: Same as Fig. 3, but now for a mass ratio of $\mu = 0.3$ and distance ratios of ${\rho _0} = 0.277$ , 0.400, 0.474, and 0.610.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F5.eps}\end{figure}$ Figure 5: Same as Fig. 3, but now for a mass ratio of $\mu = 0.1$ and distance ratios of ${\rho _0} = 0.395$ , 0.461, 0.634, and 0.670.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,height=8cm]{09758F6.eps}\end{figure}$ Figure 6: Limits of stability for planetary orbits for different mass ratios $\mu$ . We show the results based on Jacobi's constant C₁ (solid line) (criterion of stability) and based on Jacobi's constant C₂ (dashed line) and C₃ (dash-dotted line). In addition, we indicate the model parameters $\mu$ and $\rho _0$ of the simulations depicted in Figs. 3 to 5. Here the filled and open boxes refer to case studies of orbital stability and instability, respectively. The gray area indicates the domain of quasi-stability, tentatively determined by our model simulations.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\includegraphics[width=3.7cm,height=3.5cm]{09758F1a.eps... ...ce*{3mm} \includegraphics[width=3.7cm,height=3.5cm]{09758F1b.eps} } \end{figure}$	Figure 1: Setup for the circular restricted three body problem.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.5cm,height=6.5cm]{09758F2.eps}\end{figure}$	Figure 2: Locations of the Lagrange points L₁, L₂, L₃, L₄, and L₅ in synodic coordinates $X^{\ast }$ and $Y^{\ast }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F3.eps}\end{figure}$	Figure 3: For a mass ratio of $\mu = 0.5$ , runs for four different distance ratios are shown, which are ${\rho _0} = 0.200$ , 0.300, 0.425, and 0.450 (solid lines). We also show the zero velocity contours (dash-dotted lines) indicating the permitted regions of motion and the Lagrange points (crosses).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F4.eps}\end{figure}$	Figure 4: Same as Fig. 3, but now for a mass ratio of $\mu = 0.3$ and distance ratios of ${\rho _0} = 0.277$ , 0.400, 0.474, and 0.610.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{aa09758F5.eps}\end{figure}$	Figure 5: Same as Fig. 3, but now for a mass ratio of $\mu = 0.1$ and distance ratios of ${\rho _0} = 0.395$ , 0.461, 0.634, and 0.670.
Open with DEXTER