lly this is not a defition of stability， but of stability we defe a syste as beg unstable when a close enunter ours sowherethe syste， startg fro a certa itial nfiguration (chabers， wetherill ≈ap;ap;ap; boss 1996; ito ≈ap;ap;ap; tanikawa 1999) a syste is defed as experiencg a close enunter when o bodies approach one another with an area of the rger hill radi otherwise the syste is defed as beg stable henceforward we state that our pary syste is dynaically stable if no close enunter happens durg the age of our sor syste， about ±5 gyr cidentally， this defition ay be repced by onewhich an ourrence of any orbital crossg beeen either of a pair of ps takes pce this is becae we know fro experience that an orbital crossg is very likely to lead to a close enunterpary and proary systes (yoshaga， kokubo ≈ap;ap;ap; ako 1999) of urse this statent cannot be siply applied to systes with stable orbital resonances such as the neptune–pto syste

12previo studies and ais of this research

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