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Fig. 2.

image

Evolution of the octupolar efficiency parameter ϵ (Eq. (8)) as a function of the asteroid belt semi-major axis aast and the companion semi-major axis ac (left), and the companion eccentricity ec and ratio of asteroid belt semi-major axis aast and companion semi-major axis ac (right). The solid black lines delimit the regions where the octupolar regime of the three-body dynamic is expected to be dominant ϵ = 0.1 and ϵ = 10−3, and where a transition from octupolar regime to quadrupolar regime is expected to take place ϵ = 10−4.

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