2006MNRAS.368.1599V

The binary star system γ Cephei is unusual in that it harbours a stable giant planet around the larger star at a distance only about a tenth of that of the stellar separation. Numerical simulations are carried out into the stability of test particles in the system. This provides possible locations for additional planets and asteroids. To this end, the region interior to the planet is investigated in detail and found to permit structured belts of particles. The region between the planet and the secondary star, however, shows almost no stability. The existence of an Edgeworth-Kuiper belt analogue is found to be a possibility beyond 65 au from the barycentre of the system, although it shows almost no structural features. Finally, the region around the secondary star is studied for the first time. Here, a zone of stability is seen out to 1.5 au for a range of inclinations. In addition, a 10-Jupiter-mass planet is shown to remain stable about this smaller star, with the habitability and observational properties of such an object being discussed.