Astronomy & Astrophysics

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig1.eps}\vspace*{3mm} \includegraphics[width=7.8cm,clip]{5196fig2.eps} \end{figure}$ Figure 1: Top: time evolution of the resonant angle $\Theta _1$ obtained by numerical integration using the initial conditions of Table 1. Bottom: the corresponding evolution of the eccentricities.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig3.eps} \end{figure}$ Figure 2: The behavior of the semi-major axes and eccentricities during an adiabatic migration with $\tau _a=2$ $\times$ 10³ years and K=5. The migration is stopped between 2 $\times$ 10³ and 3 $\times$ 10³ years by applying a linear reduction.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig4.eps} \end{figure}$ Figure 3: The behavior of the eccentricities obtained by suddenly stopping the migration of the outer planet.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig5.eps} \includegrap... ...clip]{5196fig6.eps} \includegraphics[width=7.8cm,clip]{5196fig7.eps}\end{figure}$ Figure 4: Time evolution of the eccentricities ( top), resonant angles $\Theta _1$ ( middle) and $\Delta \varpi$ ( bottom) of the inward migrating giant planets, before and after a scattering event with an inner low mass planet.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig8.eps} \end{figure}$ Figure 5: The behavior of the eccentricities before and after a scattering with a small mass planet migrating inward from outside starting from a=2.6 AU.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig1.eps}\vspace*{3mm} \includegraphics[width=7.8cm,clip]{5196fig2.eps} \end{figure}$	Figure 1: Top: time evolution of the resonant angle $\Theta _1$ obtained by numerical integration using the initial conditions of Table 1. Bottom: the corresponding evolution of the eccentricities.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig3.eps} \end{figure}$	Figure 2: The behavior of the semi-major axes and eccentricities during an adiabatic migration with $\tau _a=2$ $\times$ 10³ years and K=5. The migration is stopped between 2 $\times$ 10³ and 3 $\times$ 10³ years by applying a linear reduction.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig4.eps} \end{figure}$	Figure 3: The behavior of the eccentricities obtained by suddenly stopping the migration of the outer planet.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig5.eps} \includegrap... ...clip]{5196fig6.eps} \includegraphics[width=7.8cm,clip]{5196fig7.eps}\end{figure}$	Figure 4: Time evolution of the eccentricities ( top), resonant angles $\Theta _1$ ( middle) and $\Delta \varpi$ ( bottom) of the inward migrating giant planets, before and after a scattering event with an inner low mass planet.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{5196fig8.eps} \end{figure}$	Figure 5: The behavior of the eccentricities before and after a scattering with a small mass planet migrating inward from outside starting from a=2.6 AU.
Open with DEXTER