hat 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 a narrow region both in time and frequency domain， though planetary motions are stochastic. since the purpose of this paper is to exhibit and overview the results of our long-term numerical integrations， we show typical example figures as evidence of the very
对火星轨道变化问题的最后解释(11/49)