All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7876f1.eps}\end{figure}$ Figure 1: Orbital evolution of the planets around the primary star of the binary (plot a) under the perturbations of the companion star, in turn affected by the gravitational pull of the outer singleton star (plot b). The initial semimajor axis of the binary is 70 AU, the eccentricity of the binary 0.2, that of the singleton 0.2, and the mutual inclination $i_{\rm m}$ is set to $90^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7876f2.eps}\end{figure}$ Figure 2: Same as in Fig. 1 but for a lower value of $i_{\rm m}$ set to $30^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7876f3_1.eps}\par\includeg... ...p]{7876f3_2.eps}\par\includegraphics[width=7.8cm,clip]{7876f3_3.eps}\end{figure}$ Figure 3: Destabilization of planets around the primary when the singleton is on a retrograde orbit relative to the companion. The initial mutual inclination between the two outer stars is $150^{\circ }$ . The $\Delta \Omega$ angle librates around $180^{\circ }$ while the inclinations of the two planets have wide oscillations. Only two planets, the closer ones, survive after 1 Myr ofevolution.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7876f4.eps}\end{figure}$ Figure 4: Fraction $P_{\rm s}$ of binaries that, at the end of the temporary triple phase, retain at least one of the planets in a stable orbit around the primary vs. $i_{\rm m}$ , the initial mutual inclination between the singleton and the binary companion.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7876f5.eps}\end{figure}$ Figure 5: Fraction $P_{\rm s}$ of binaries that, at the end of the temporary triple phase, retain at least one of the planets in a stable orbit around the primary vs. $a_{\rm b}$ , the binary semimajor axis. The mutual inclination $i_{\rm m}$ is set to $90^{\circ }$ , the worst case for planet stability.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7876f2.eps}\end{figure}$	Figure 2: Same as in Fig. 1 but for a lower value of $i_{\rm m}$ set to $30^{\circ }$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7876f4.eps}\end{figure}$	Figure 4: Fraction $P_{\rm s}$ of binaries that, at the end of the temporary triple phase, retain at least one of the planets in a stable orbit around the primary vs. $i_{\rm m}$ , the initial mutual inclination between the singleton and the binary companion.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7876f5.eps}\end{figure}$	Figure 5: Fraction $P_{\rm s}$ of binaries that, at the end of the temporary triple phase, retain at least one of the planets in a stable orbit around the primary vs. $a_{\rm b}$ , the binary semimajor axis. The mutual inclination $i_{\rm m}$ is set to $90^{\circ }$ , the worst case for planet stability.
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