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Despite the discovery of thousands of exoplanets in recent years, the numberof known exoplanets in star clusters remains tiny. This may be a consequence ofclose stellar encounters perturbing the dynamical evolution of planetarysystems in these clusters. Here, we present the results from direct $N$-bodysimulations of multiplanetary systems embedded in star clusters containing $N =8k, 16k, 32k$, and $64k$ stars. The planetary systems, which consist of thefour Solar system giant planets Jupiter, Saturn, Uranus, and Neptune, areinitialized in different orbital configurations, to study the effect of thesystem architecture on the dynamical evolution of the entire planetary system,and on the escape rate of the individual planets. We find that the currentorbital parameters of the Solar system giants (with initially circular orbits,as well as with present-day eccentricities) and a slightly more compactconfiguration, have a high resilience against stellar perturbations. Aconfiguration with initial mean-motion resonances of 3:2, 3:2, and 5:4 betweenthe planets, which is inspired by the Nice model, and for which the twooutermost planets are usually ejected within the first $10^5$ yr, is in manycases stabilized due to the removal of the resonances by external stellarperturbation and by the rapid ejection of at least one planet. Assigning allplanets the same mass of 1 Jovian mass almost equalizes the survival fractions.Our simulations reproduce the broad diversity amongst observed exoplanetsystems. We find not only many very wide and/or eccentric orbits, but also asignificant number of (stable) retrograde orbits.

On the survival of resonant and non-resonant planetary systems in star clusters