Dynamical evolution of a young planetary system: stellar flybys in co-planar orbital configuration
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ORIGINAL ARTICLE
Dynamical evolution of a young planetary system: stellar flybys in co-planar orbital configuration Raffaele Stefano Cattolico1
· Roberto Capuzzo-Dolcetta1
Received: 14 July 2020 / Accepted: 17 October 2020 © Springer Nature B.V. 2020
Abstract Stellar flybys in star clusters may perturb the evolution of young planetary systems in terms of disk truncation, planetary migration and planetary mass accretion. We investigate the feedback of a young planetary system during a single close stellar encounter in a typical open young stellar cluster. We consider 5 masses for the stellar perturbers: 0.5, 0.8, 1, 3 and 8 M , in coplanar, prograde and retrograde orbits respect to the planetary disk, varying the perturberhost star orbital periastron from 100 au to 500 au. We have made 3D modelizations with the smooth particle hydrodynamics code GaSPH of a system composed by a solar type star surrounded by a low density disk where a giant planet is embedded in. We focus on the dynamical evolution of global parameters characterizing the disk and the planet, like the Lagrangian radius containing the 63.2% of the mass of the disk, the distance of the planet to its host star, the planet orbital eccentricity and the planetary mass accretion. We find that the most part of the simulated systems show a significant disk truncation after a single close encounter, a final orbital distance of the Jovian, from the central star, lower than the unperturbed case and, finally, the perturbed systems show a final mass accretion of the Jovian planet larger than the non-perturbed case. Therefore, stellar flybys significantly perturb the dynamics of a young planetary system, regardless the orbital configuration of the stellar perturber. In such experiments, the final disk radius and the orbital parameters of the Jovian planet are considerably affected by the stellar close encounter. Keywords Planets and satellites: dynamical evolution and stability · Planet-disk interactions · Methods: numerical
B R.S. Cattolico 1
Dep. of Physics, Sapienza, Univ. of Rome, P.le A. Moro 5, 00185 Rome, Italy
1 Introduction Stars tend to form in stellar aggregates or clusters (Hillenbrand 1997; Palla and Stahler 2000), even our Sun might have formed this way (Dukes and Krumholz 2012). Consequently, the planetary architectures around stars have likely been affected by several stellar gravitational interactions (Picogna and Marzari 2014; Rosotti et al. 2014; Cuello et al. 2018). If the planetary system is aged in the interval 3– 12 Myr, it, likely, still shows a circumstellar disk (Haisch et al. 2001). Moreover, a coexistence between a forming planet and the gaseous disk is predicted both by theoretical models (Pollack et al. 1996) and observations, as shown by several surveys obtained by instruments like SPHERE (Avenhaus et al. 2014) through a direct imaging in the nearinfrared, or in radio bands by ALMA (Andrews et al. 2018). Several studies have simulated circumstellar disks using different approaches, starting from a clump of “test particles” to a fu
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