对火星轨道变化问题的最后解释(1/12)
作者君在作品相关中其实已经解释过这个问题。
不过仍然有人质疑。
那么作者君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-termiionsandstabilityofparyorbitsinourSorsystem
Abstract
Wepresenttheresultsofverylong-termnumericaliionsofparyorbitalmotionsover109-yrtime-spansincludingallnineps.Aquispeofournumericaldatashowsthattheparymotion，atleastinoursimpledynamicalmodel，seemstobequitestableevehisverylongtime-span.Acloserlookatthelowest-frequencyosciltionsusingalow-passfiltershowsusthepotentiallydiffusivecharacterofterrestrialparymotion，especiallythatofMercury.ThebehaviouroftheetriercuryinouriionsisqualitativelysimirtotheresultsfromJacquesLaskar''''''''ssecurperturbationthe.emax～0.35yr.However，therearenoapparentsecreasesofetricityorinationinanyorbitalelementsoftheps，whichmayberevealedbystillloermnumericaliions.Wehavealsoperformedacoupleoftrialiionsincludingmotionsoftheouterfivepsoverthedurationof±5×1010yr.Theresultindicatesthatthethreemajorresoheune–Plutosystemhavebeenmaintainedoverthe1011-yrtime-span.
1Introdu
1.1Definitionoftheproblem
ThequestionofthestabilityofourSorsystemhasbeeedoverseveralhundredyears，siheeraofon.Theproblemhasattractedmanyfamousmathematisovertheyearsandhaspyedatralroleinthedevelopmentofnon-lineardynamidchaostheory.However，wedohaveadefihequestionofwhetherourSorsystemisstableornot.Thisispartlyaresultofthefactthatthedefinitionoftheterm‘stability’isvaguewhenitisusediiontotheproblemofparymotionintheSorsystem.Actuallyitisogiveaclear，rigorousandphysicallymeaningfuldefinitionofthestabilityofourSorsystem.
Amongmanydefinitionsofstability，herettheHilldefinitionGdman1993:actuallythisisnotadefinitionofstability，butofinstability.Wedefineasystemasbeingunstablewhenacloseenteroccurssomewhereiem，startingfromacertaininitialfigurationChambers，Wetherill&Boss1996;Ito&Tanikawa1999.AsystemisdefinedasexperiengacloseenterwhentwobodiesapproaeahinahergerHillradius.Otherwisethesystemisdefinedasbeingstable.Henceforwardwestatethatourparysystemisdynamicallysta
不过仍然有人质疑。
那么作者君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-termiionsandstabilityofparyorbitsinourSorsystem
Abstract
Wepresenttheresultsofverylong-termnumericaliionsofparyorbitalmotionsover109-yrtime-spansincludingallnineps.Aquispeofournumericaldatashowsthattheparymotion，atleastinoursimpledynamicalmodel，seemstobequitestableevehisverylongtime-span.Acloserlookatthelowest-frequencyosciltionsusingalow-passfiltershowsusthepotentiallydiffusivecharacterofterrestrialparymotion，especiallythatofMercury.ThebehaviouroftheetriercuryinouriionsisqualitativelysimirtotheresultsfromJacquesLaskar''''''''ssecurperturbationthe.emax～0.35yr.However，therearenoapparentsecreasesofetricityorinationinanyorbitalelementsoftheps，whichmayberevealedbystillloermnumericaliions.Wehavealsoperformedacoupleoftrialiionsincludingmotionsoftheouterfivepsoverthedurationof±5×1010yr.Theresultindicatesthatthethreemajorresoheune–Plutosystemhavebeenmaintainedoverthe1011-yrtime-span.
1Introdu
1.1Definitionoftheproblem
ThequestionofthestabilityofourSorsystemhasbeeedoverseveralhundredyears，siheeraofon.Theproblemhasattractedmanyfamousmathematisovertheyearsandhaspyedatralroleinthedevelopmentofnon-lineardynamidchaostheory.However，wedohaveadefihequestionofwhetherourSorsystemisstableornot.Thisispartlyaresultofthefactthatthedefinitionoftheterm‘stability’isvaguewhenitisusediiontotheproblemofparymotionintheSorsystem.Actuallyitisogiveaclear，rigorousandphysicallymeaningfuldefinitionofthestabilityofourSorsystem.
Amongmanydefinitionsofstability，herettheHilldefinitionGdman1993:actuallythisisnotadefinitionofstability，butofinstability.Wedefineasystemasbeingunstablewhenacloseenteroccurssomewhereiem，startingfromacertaininitialfigurationChambers，Wetherill&Boss1996;Ito&Tanikawa1999.AsystemisdefinedasexperiengacloseenterwhentwobodiesapproaeahinahergerHillradius.Otherwisethesystemisdefinedasbeingstable.Henceforwardwestatethatourparysystemisdynamicallysta
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