e variation of planetary orbital elements does not differ significantly between the initial and final part of each integration， at least for venus， earth and mars. the elements of mercury， especially its eccenicity， seem to change to a significant extent. this is partly because the orbital time-scale of the planet is the shortest of all the planets， which leads to a more rapid orbital evolution than other planets; the innermost planet may be nearest to instability. this result appears to be in some agreement with laskar's (1994， 1996) expectations that large and irregular variations appear in the eccenicities and inclinations of mercury on a time-scale
对火星轨道变化问题的最后解释(25/49)