Evolution of the orbital separation (top) and eccentricity (bottom) for the selected star in fig. D.1, but now with six planets between 1 au and 180 au according to an Oligarchic planet-formation model (Kokubo & Ida 1998). The planetary system was integrated for 7 Myr, while the 6 nearest stars were taken into account in the gray-shaded areas. The initial planetary system would have been stable if it evolved in isolation, but the perturbations caused several planets to change their orbits considerably. Most noticeable is the high increase in eccentricity to 0.31 of the outermost planet due to the encounter that kicked the star from the cluster (see Fig. D.1). An earlier encounter at 3.8 Myr already affected the outer planet’s orbit.