对火星轨道变化问题的最后解释(第4/16页)
integrations.
in this paperpresent prelinary resultssix longternbsp;nurical integrationsall nine plary orbits， coverinpanseveral 109 yr， andtwo other integrations coverinpan of51010 yr. the total elapsedfor all integrationsre than 5 yr， using several dedicated pcsof the fundantal conclusionsour longternbsp;integrationsthat solar systenbsp;plary tion seebe stableterthe hill stability ntioned above，least oveispan of，our nurical integrations the systenbsp;was farstable than whatdefinedthe hill stability criterion: not only didclose encounter happen during the integration period， but also all the plary orbital elents have been confineda narrow region bothti and frequency doin， though plary tionsthe purposethis paperto exhibit and overview the resultsour longternbsp;nurical integrations，show typical exale figuresevidencethe very longternbsp;stabilitysolar systenbsp;plar readers who havespecific and deeper interestsour nurical results，have prepareebpa ess ， whereshow raw orbital elents， their lowpass filtered results， variationdelaunay elents and angular ntunbsp;deficit， and resultsour sile ti–frequency analysisallour integrations.
in section 2briefly explain our dynacal del， nurical thod and initial conditions usedou 3devoteda descriptionthe quick resultsthe nurica longternbsp;stabilitysolar systenbsp;plary tionapparent bothplary positions and orbita estitionnurical errorsals 4 goestiscussionthe lonstternbsp;variationplary orbits usinowpass filter and includeiscussionangular ntunbsp; section 5，presenetnurical integrations for the outer five pls that spans51010 yr.s
本章未完，请点击下一页继续阅读 》》
in this paperpresent prelinary resultssix longternbsp;nurical integrationsall nine plary orbits， coverinpanseveral 109 yr， andtwo other integrations coverinpan of51010 yr. the total elapsedfor all integrationsre than 5 yr， using several dedicated pcsof the fundantal conclusionsour longternbsp;integrationsthat solar systenbsp;plary tion seebe stableterthe hill stability ntioned above，least oveispan of，our nurical integrations the systenbsp;was farstable than whatdefinedthe hill stability criterion: not only didclose encounter happen during the integration period， but also all the plary orbital elents have been confineda narrow region bothti and frequency doin， though plary tionsthe purposethis paperto exhibit and overview the resultsour longternbsp;nurical integrations，show typical exale figuresevidencethe very longternbsp;stabilitysolar systenbsp;plar readers who havespecific and deeper interestsour nurical results，have prepareebpa ess ， whereshow raw orbital elents， their lowpass filtered results， variationdelaunay elents and angular ntunbsp;deficit， and resultsour sile ti–frequency analysisallour integrations.
in section 2briefly explain our dynacal del， nurical thod and initial conditions usedou 3devoteda descriptionthe quick resultsthe nurica longternbsp;stabilitysolar systenbsp;plary tionapparent bothplary positions and orbita estitionnurical errorsals 4 goestiscussionthe lonstternbsp;variationplary orbits usinowpass filter and includeiscussionangular ntunbsp; section 5，presenetnurical integrations for the outer five pls that spans51010 yr.s
本章未完，请点击下一页继续阅读 》》