Formation of Wide-orbit Gas Giants Near the Stability Limit in Multi-stellar Systems

Abstract

We have investigated the formation of a circumstellar wide-orbit gas giant planet in a multiple stellar system. We consider a model of orbital circularization for the core of a giant planet after it is scattered from an inner disk region by a more massive planet, which was proposed by Kikuchi et al. We extend their model for single star systems to binary (multiple) star systems, by taking into account tidal truncation of the protoplanetary gas disk by a binary companion. As an example, we consider a wide-orbit gas giant in a hierarchical triple system, HD131399Ab. The best-fit orbit of the planet is that with semimajor axis ∼80 au and eccentricity ∼0.35. As the binary separation is ∼350 au, it is very close to the stability limit, which is puzzling. With the original core location ∼20–30 au, the core (planet) mass ∼50 M E and the disk truncation radius ∼150 au, our model reproduces the best-fit orbit of HD131399Ab. We find that the orbit after the circularization is usually close to the stability limit against the perturbations from the binary companion, because the scattered core accretes gas from the truncated disk. Our conclusion can also be applied to wider or more compact binary systems if the separation is not too large and another planet with ≳20–30 Earth masses that scattered the core existed in inner region of the system.