edicated pcs and workstations. one of the fundamental conclusions of our long-term integrations is that solar system planetary motion seems to be stable in terms of the hill stability mentioned above， at least over a time-span of ± 4 gyr. actually， in our numerical integrations the system was far more stable than what is defined by the hill stability criterion: not only did no close encounter happen during the integration period， but also all the planetary orbital elements have been confined in
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