(1) Xi’An Jiaotong-Liverpool University ; (2) Leiden university; (3) Chinese Academy of Sciences; (4) Kavli Institute for Astronomy and Astrophysics at Peking University; (5) Zentrum für Astronomie der Universität Heidelberg Abstract Most stars in the Galaxy form in stellar groupings that either dissolve within several tens of millions of years, or evolve into open clusters. It is important to study the dynamics of planetary systems in such structures to explain the properties of observed exoplanets. Here, we numerically evolve open star clusters with planetary systems by combining the star cluster code NBODY6++GPU code with the planetary system code REBOUND. We use different sets of initial conditions, such as the virial ratio and stellar density, and evolve the system for 50 Myr. We find that stellar encounter properties, the star cluster density, and the planetary system architecture are the main factors that affect the evolution of the planetary systems. Although most planetary systems remain intact, others lose most of their outer planets, while some are stripped of all planets. Finally, we find that the presence of the planet Jupiter plays a prominent role in the survival chances of terrestrial planets. References [1] Lada 2003, A&A, 03011540 [2]Rein and Liu 2012, A&A 537, A128 [3] Wang, Spurzem et al,2015, MNRAS 450, 4070–4080 [4] Cai et al 2015, ApJ, 1506.0759 [5] hdfgroup.org [6] Cai et al 2017, 1706.03789 [7]Flammini Dotti et al 2020a [8]Flammini Dotti et al,2019 [9] Fujii et al 2019, A&A, 624, A110 [10]Flammini Dotti et al 2020b Initial Conditions Star Clusters: N= 500, 5000, 10000 stars; Q = 0.4,0.5,0.6; Rcluster = 1 pc; IMF Kroupa (2001), Plummer sphere, Standard Galactic Tidal Field Planetary Systems: ~1 MSun Host,: 6 planets (Earth, Mars and four gas giants), no protoplanetary disk, number of planetary system per star cluster, respectively, 25, 125, 200 Conclusions and Discussion We have carried out a set of N-body simulation in order to understand the influence of the star cluster on a Solar system-like planetary system. Most planetary system remain stable during the whole simulation, while most of the unstable one have ejected the outermost planets. The terrestrial planets are ejected mostly if Jupiter orbits gets perturbed, and it is completely destroyed with a impulsive encounter[8] . In the presence of a encounter, Jupiter acts both as dynamical barrier for weak encounters and as a perturber for the terrestrial planet for stronger encounters-. The final architecture of planets can be seen in the table, where the 1 and 2 planetary system are always, for all simulation and initial conditions, Jupiter for the 1 planet Solar system and Jupiter and Saturn for the 2 planet Solar system. The three planets scenario is unlikely for the empirical consequence of the Saturn presence in the 2-planets system. Black holes have also shown to impact the ejection of planets from their stellar systems[10]. Methodology We use REBOUND[2 ] as integrator for planetary systems and NBODY6++GPU [3] for the star cluster in order to model the gravitational dynamics, via N-Body codes, of both. The latter is using a C code environment, also working along with Python, optimised for few-body integrations, while the last is optimised for highly accurate and fast calculation and also supports MPI and GPU implementations, built for many-body integrations. We used 50 Myr as an evolutionary time, while 1000 years is the time-step for the star cluster output. The planetary output time-step is adaptive, and reproduces the previous 1000 years time-steps in the data storage, while it warns the user if the planets either escape or merge during this period (in short block time storage[4] ). We use the HDF5 format, which allows us to store data with high temporal resolution.[5] Finally the simulation can be resumed in 3 principal steps: star cluster and planetary system initial conditions, stars gravitational evolution with the nearby stars and plane