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Secular instability in the spatial three-body problem

dc.contributor.authorFéjoz, Jacques
dc.contributor.authorGuardia, Marcel
dc.date.accessioned2017-11-30T09:59:06Z
dc.date.available2017-11-30T09:59:06Z
dc.date.issued2016
dc.identifier.issn0003-9527
dc.identifier.urihttps://basepub.dauphine.fr/handle/123456789/17111
dc.language.isoenen
dc.subjectsystèmes dynamiques
dc.subjectthree-body problem
dc.subject.ddc515en
dc.titleSecular instability in the spatial three-body problem
dc.typeArticle accepté pour publication ou publié
dc.description.abstractenConsider the spatial three-body problem, in the regime where one bodyrevolves far away around the other two, in space, the masses of the bodies being arbi-trary but fixed; in this regime, there are no resonances in mean motions. The so-calledsecular dynamics governs the slow evolution of the Keplerian ellipses. We show thatit contains a horseshoe and all the chaotic dynamics which goes along with it, corre-sponding to motions along which the eccentricity of the inner ellipse undergoes large,random excursions. The proof goes through the surprisingly explicit computation of thehomoclinic solution of the first order secular system, its complex singularities and theMelnikov potential.
dc.relation.isversionofjnlnameArchive for Rational Mechanics and Analysis
dc.relation.isversionofjnlvol221
dc.relation.isversionofjnlissue1
dc.relation.isversionofjnldate2016
dc.relation.isversionofjnlpages335–362
dc.relation.isversionofdoi10.1007/s00205-015-0962-y
dc.relation.isversionofjnlpublisherSpringer
dc.subject.ddclabelAnalyseen
dc.relation.forthcomingnonen
dc.relation.forthcomingprintnonen
dc.description.ssrncandidatenon
dc.description.halcandidatenon
dc.description.readershiprecherche
dc.description.audienceInternational
dc.relation.Isversionofjnlpeerreviewedoui
dc.date.updated2017-12-19T09:51:24Z


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