对火星轨道变化问题的最后解释(第3/16页)
s longternbsp;nurical integrations included only the outer five pls sussn & wisdonbsp;1988; kinoshita & nakabecause the orbital periodsthe outer pls arech lonr than thosethe inner four pls thatiseasierfollow the systenbsp;foiven integratio present， the lonst nurical integrations publishedjournals are thoseduncan & lissaue theirtart was the effectpostinsequence solarlossthe stabilityplary orbits， they perfordintegrations coveringto 1011of the orbital tionsthe four jovia initial orbital elents and ssespls are theas thoseour solar systenbsp;in duncan & lissauer&039;s paper， but they decrease theof the sun graduallytheir nuricabecause they consider the effectpostinsequence solarlossth， they found that the crossing tiscaleplary orbits， which cana typical indicatorthe instability tiscale，quite sensitivethe ratess decreaseth theof the suncloseits present value， the jovian pls rein stable over 1010 yr，perhap & lissauer also perford four silar experintsthe orbital tionseven pls venusneptune， which covepan109 yr. their experintsthe seven pls are not yet&nbspprehensive， butsee that the terrestrial pls also rein stable during the integration period， intaining alst regular oscillations.
on the other hand，his urate seanalytical secular perturbation theory laskar 1988， laskar finds that lar and irregular variations can appearthe entricities and inclinationsthe terrestrial pls， especiallymercury and marsa tiscaleseveral 109laska resultslaskar&039;s secular perturbation theory shouldconfird and investigatedfully nurical
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on the other hand，his urate seanalytical secular perturbation theory laskar 1988， laskar finds that lar and irregular variations can appearthe entricities and inclinationsthe terrestrial pls， especiallymercury and marsa tiscaleseveral 109laska resultslaskar&039;s secular perturbation theory shouldconfird and investigatedfully nurical
本章未完，请点击下一页继续阅读 》》