Hill-Type Stability and Hierarchical Stability of the General Three-Body Problem
none of the bodies escapes to infinity from the system;
no dramatic changes occur in any orbit’s size, shape or orientation to the invariable plane of the system;
ρi < ρj for any i < j; where ρi = |ρi| (i=2,..., N), ρi being the Jacobian vectors which connect the barycentre of the first (i-1) masses and the ith mass.
KeywordsJacobian Vector Synodic Period Invariable Plane Negative Total Energy Outer Mass
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