对火星轨道变化问题的最后解释(第7/16页)
etheir preservatioota good asurethe uracynurical integrations， especiallya asurethe positional errorpls， i.e. the errorplar estite the nurical errorthe plary longitudes，perford the followin&nbsppared the resultourlongternbsp;integrations withtest integrations， which spanshorter periods but withhigher uracy than thhis purpose，perford are urate integration with a d 164theintegrations spanning 3105 yr， starting with theinitial conditionsin thonsider that this test integration provideswitseudotrue solutionplary orbita， we&nbsppare the test integration with theintegration， n1. for the period3105 yr，seifferencean anoliesthe earth between the two the casethifference canextrapolatedthe value 8700， aboutrotationsearth after 5 gyr， since the errorlongitudes increases linearly within the sylectic p. silarly， the longitude errorpluto canestited12. this value for plutoch better than the resultkinoshita & nakai 1996 where the differenceestited60.
3 nurical results – i. glancethe raw data
in this sectionbriefly review the longternbsp;stabilityplary orbital tion throughsnapshotsraw nurica orbital tionpls indicates longternbsp;stabilityallour nurical integrations:orbital crossings nor close encounters between any pairpls took place.
3.1 neral descriptionthe stabilityplary orbits
first，briefly lookthe neral characterthe longternbsp;stabilityplar interest here focuses particularlythe inner four terrestrial pls for which the orbital tiscales areshorter than thosethe outer fivcan see clearly fronbsp;the planar orbital configurations shownfig
本章未完，请点击下一页继续阅读 》》
3 nurical results – i. glancethe raw data
in this sectionbriefly review the longternbsp;stabilityplary orbital tion throughsnapshotsraw nurica orbital tionpls indicates longternbsp;stabilityallour nurical integrations:orbital crossings nor close encounters between any pairpls took place.
3.1 neral descriptionthe stabilityplary orbits
first，briefly lookthe neral characterthe longternbsp;stabilityplar interest here focuses particularlythe inner four terrestrial pls for which the orbital tiscales areshorter than thosethe outer fivcan see clearly fronbsp;the planar orbital configurations shownfig
本章未完，请点击下一页继续阅读 》》