All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{9453f1.eps} \end{figure}$ Figure 1: This figure shows the initial disc surface density profile. The initial position of the planet with mass of $m_{\rm p}=20~M_\oplus$ is represented by a black circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{9453f2.eps}\vspace*{3mm} \includegraphics[width=7.3cm,clip]{9453f3.eps} \end{figure}$ Figure 2: This figure shows the mass of the planet as a function of time for simulations in which $t_{\rm acc}=t_{\rm dyn}$ ( upper panel) and $t_{\rm acc}=10~t_{\rm dyn}$ ( lower panel). The dotted (resp. dashed) line corresponds to simulations in which the final mass of the planet is 1 $M_{\rm s}$ (resp. 1 $M_{\rm J}$ ). In simulations represented by the solid line, the final mass of the planet is not imposed.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9453f4.eps}\hspace*{4mm} \includegraphics[width=7.6cm,clip]{9453f5.eps} \end{figure}$ Figure 3: This figure shows the evolution of the system for models in which $m_{\rm p}=1~M_{\rm S}$ . Here, the left and right panels correspond to $t_{\rm acc}=t_{\rm dyn}$ and $t_{\rm acc}=10~t_{\rm dyn}$ respectively. Top: evolution of the semi-major axis of the planet. Middle: evolution of the eccentricities for the planet (black), binary (red) and disc (green). Bottom: evolution of the longitudes of pericentre for the planet (black), binary (red) and disc (green).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{9453f6.eps} \end{figure}$ Figure 4: This figure shows, over a few planetary orbital periods, the evolution of the torques exerted by the disc on the planet (solid line) as well as the time evolution of the orbital the position of the planet $r_{\rm p}$ (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f7.eps}\hspace*{3mm} \... ...f9.eps}\hspace*{3mm} \includegraphics[width=5.2cm,clip]{9453f10.eps}\end{figure}$ Figure 5: This figure shows, for the model in which $m_{\rm p}=1~M_{\rm S}$ and $t_{\rm acc}=t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9453f11.eps}\hspace*{4mm} \includegraphics[width=7.6cm,clip]{9453f12.eps} \end{figure}$ Figure 6: This figure shows the evolution of the system for models in which $m_{\rm p}=1~M_{\rm J}$ . Here, the left and right panels correspond to $t_{\rm acc}=t_{\rm dyn}$ and $t_{\rm acc}=10~t_{\rm dyn}$ respectively. Top: evolution of the semi-major axis of the planet. Middle: evolution of the eccentricities for the planet (black), binary (red) and disc (green). Bottom: evolution of the longitudes of pericentre for the planet (black), binary (red) and disc (green).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{9453f13.eps} \end{figure}$ Figure 7: This figure shows, for the simulation with $m_{\rm p}=1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , the evolution of the resonant angles $\psi _1$ , $\psi _2$ , $\psi _3$ and $\psi _4$ associated with the 4:1 resonance.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f14.eps}\hspace*{3mm} ... ....eps}\hspace*{3mm} \includegraphics[width=5.2cm,clip]{9453f17.eps} \end{figure}$ Figure 8: This figure shows, for the model in which $m_{\rm p}=1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9453f18.eps}\hspace*{4mm} \includegraphics[width=7.6cm,clip]{9453f19.eps} \end{figure}$ Figure 9: This figure shows the evolution of the system for models in which $m_{\rm p} > 1~M_{\rm J}$ . Here, the left and right panels correspond to $t_{\rm acc}=t_{\rm dyn}$ and $t_{\rm acc}=10~t_{\rm dyn}$ respectively. Top: evolution of the semi-major axis of the planet. Middle: evolution of the eccentricities for the planet (black), binary (red) and disc (green). Bottom: evolution of the longitudes of pericentre for the planet (black), binary (red) and disc (green).
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9453f20.eps} \end{figure}$ Figure 10: This figure shows, for the simulation with $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , the evolution of the resonant angles $\psi _1$ , $\psi _2$ , $\psi _3$ and $\psi _4$ associated with the 4:1 resonance.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f21.eps}\hspace*{3mm} ... ....eps}\hspace*{3mm} \includegraphics[width=5.2cm,clip]{9453f24.eps} \end{figure}$ Figure 11: This figure shows, for the model in which $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=10~t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9453f25.eps} \end{figure}$ Figure 12: This figure shows, for the model with $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=10~t_{\rm dyn}$ , the evolution of the torques exerted by the disc on the planet. The blue (red) line corresponds to the inner (outer) disc torques and the black line corresponds to the net torques exerted on the planet.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{9453f1.eps} \end{figure}$	Figure 1: This figure shows the initial disc surface density profile. The initial position of the planet with mass of $m_{\rm p}=20~M_\oplus$ is represented by a black circle.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{9453f6.eps} \end{figure}$	Figure 4: This figure shows, over a few planetary orbital periods, the evolution of the torques exerted by the disc on the planet (solid line) as well as the time evolution of the orbital the position of the planet $r_{\rm p}$ (dashed line).
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$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f7.eps}\hspace{3mm} \... ...f9.eps}\hspace{3mm} \includegraphics[width=5.2cm,clip]{9453f10.eps}\end{figure}$	Figure 5: This figure shows, for the model in which $m_{\rm p}=1~M_{\rm S}$ and $t_{\rm acc}=t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{9453f13.eps} \end{figure}$	Figure 7: This figure shows, for the simulation with $m_{\rm p}=1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , the evolution of the resonant angles $\psi _1$ , $\psi _2$ , $\psi _3$ and $\psi _4$ associated with the 4:1 resonance.
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$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f14.eps}\hspace{3mm} ... ....eps}\hspace{3mm} \includegraphics[width=5.2cm,clip]{9453f17.eps} \end{figure}$	Figure 8: This figure shows, for the model in which $m_{\rm p}=1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9453f20.eps} \end{figure}$	Figure 10: This figure shows, for the simulation with $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=t_{\rm dyn}$ , the evolution of the resonant angles $\psi _1$ , $\psi _2$ , $\psi _3$ and $\psi _4$ associated with the 4:1 resonance.
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$\begin{figure} \par\includegraphics[width=5.2cm,clip]{9453f21.eps}\hspace{3mm} ... ....eps}\hspace{3mm} \includegraphics[width=5.2cm,clip]{9453f24.eps} \end{figure}$	Figure 11: This figure shows, for the model in which $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=10~t_{\rm dyn}$ , snapshots of the disc surface density at times shown above the plots. Here, the planet is represented by a white circle.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{9453f25.eps} \end{figure}$	Figure 12: This figure shows, for the model with $m_{\rm p} > 1~M_{\rm J}$ and $t_{\rm acc}=10~t_{\rm dyn}$ , the evolution of the torques exerted by the disc on the planet. The blue (red) line corresponds to the inner (outer) disc torques and the black line corresponds to the net torques exerted on the planet.
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