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A giant planet has been recently resolved at a projected distance of 730 aufrom the tight pair of young ($\sim$ 13 Myr) intermediate-mass stars HD106906AB in the Lower Centaurus Crux (LCC) group. The stars are surrounded by adebris disk which displays a ring-like morphology and strong asymmetries atmultiple scales. We aim at studying the likelihood of a scenario where theplanet formed closer to the stars in the disk, underwent inward disk-inducedmigration, and got scattered away by the binary star before being stabilized bya close encounter (fly-by). We performed semi-analytical calculations andnumerical simulations (Swift_HJS package) to model the interactions between theplanet and the two stars. We accounted for the migration as a simple force. Westudied the LCC kinematics to set constraints on the local density of stars,and therefore on the fly-by likelihood. We performed N-body simulations todetermine the effects of the planet trajectories (ejection and secular effects)onto the disk morphology. The combination of the migration and mean-motionresonances with the binary star (often 1:6) can eject the planet. Nonetheless,we estimate that the fly-by hypothesis decreases the scenario probability toless than $10^{-7}$ for a derived local density of stars of 0.11stars/pc$^{3}$. We show that the concomitant effect of the planet and starstrajectories induce spiral-features in the disk which may correspond to theobserved asymmetries. Moreover, the present disk shape suggests that the planetis on an eccentric orbit. The scenario we explored is a natural hypothesis ifthe planet formed within a disk. Conversely, its low probability of occurrenceand the fact that HD 106906 b shares some characteristics with other systems inSco-Cen (e.g. HIP 78530, in terms of mass ratio and separation) may indicate analternative formation pathway for those objects.

On the origin of the wide-orbit circumbinary giant planet HD 106906: A dynamical scenario and its impact on the disk