第76章 对火星轨道变化问题的最后解释
作者君在作品相关中已经解释过这个问题，并在此列出相关参考文献中的一篇开源论文。
以下是文章内容：
long-terary orbits in our sr systeary orbital s. a quick inspection of our nuary ary s， which s over the duration of ± 5 x 1010 yr. the result indicates that the three ary ary systes takes ce. this is because we know froary and protory systes in our sr systeary systes for a period covering several 10 gyr to thoroughly understand the long-terary orbits， since chaotic dynas (susss are so s that it is ary orbits， they perfors. the initial orbital eles are the saary orbits， which can be a typical indicator of the instability tis res (venus to neptune)， which cover a span of 109 yr. their experis are not yet cos also res， especially of mercury and mars on a tiary orbits， covering a span of several 109 yr， and of two other integrations covering a span of ± 5 x 1010 yr. the total psed tiary ary orbital eleary ary ary ary positions and orbital eleary orbits using a low-pass filter and includes a discussion of angr s that spans ± 5 x 1010 yr. in section 6 we also discuss the long-terary s (n±1，2，3)， which is about 1/11 of the orbital period of the inner (mercury). as for the deters in sussary orbits using the sys (f±)， we fixed the stepsize at 400 d.
we adopt gauss f and g functions in the sys (n±1，2，3)， and about 8000 000 d (21 903 yr) for the integration of the outer five pls (f±).
although no output filtering was done when the nuary longitudes
since the sys， i.e. the error in ry longitudes. to estiary longitudes， we perforary orbital evolution. next， we coary orbital s indicates long-ters took ce.
3.1 general description of the stability of ry orbits
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