J/A+A/646/A182ivo://CDS.VizieR/J/A+A/646/A182doi:10.26093/cds/vizier.36460182CDSKankiewicz P.Wlodarczyk I.2021-09-06T12:33:13Z2021-02-26T07:56:08ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frsolar-systemasteroidsDynamical studies of asteroid populations in retrograde orbits, i.e. with orbital inclinations greater than 90 degrees, are interesting because the origin of such orbits is still unexplained. Generally, the retrograde asteroids population includes mostly Centaurs and transneptunian objects (TNOs). A special case is the Near Earth Object (343158) 2009 HC82 from the Apollo group. Another interesting object is the comet 333P/LINEAR, which for several years was considered as the second retrograde object approaching Earth. One more comet in retrograde orbit, 161P Hartley/IRAS appears to be an object of similar type. Thanks to the large amount of observational data for these two comets, we tested various models of cometary non-gravitational forces applied to their dynamics. The goal was to estimate which of non-gravitational perturbations could affect the stability of retrograde bodies. In principle, we study the local stability by measuring the divergence of nearby orbits. We have numerically determined Lyapunov chaotic indicators (LCI) and the associated Lyapunov times (LT). This time, our calculations of these parameters were extended by more advanced models of non-gravitational perturbations (i.e. Yarkovsky drift and in selected cases cometary forces). This allowed estimating the chaos in the Lyapunov sense. We found that the Yarkovsky effect for obliquities of gamma=0{deg} and gamma=180{deg} can change LT substantially. In most cases, for the prograde rotation, we received more stable solutions. Moreover, we confirmed the role of retrograde resonances in this process. Additionally, the studied cometary effects also significantly influence the long-term behaviour of the selected comets. LT can reach values from 100 to over 1000 years. All results indicate that the use of models with non-gravitational effects for retrograde bodies is clearly justified.2021A&A...646A.182Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/646/A182CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/646/A182https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/646/A182http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/646/A182https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/646/A182https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/646/A182http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/646/A182GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/646/A182/table4Lyapunov Times of retrograde asteroidsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameAsteroid namemeta.id;meta.mainchariInclination of orbitdegsrc.orbital.inclinationfloataSemimajor axisauphys.angSize;srcfloateEccentricitysrc.orbital.eccentricityfloatHAbsolute magnitudemagphys.magAbsfloatDDiameterkmphys.angSizefloatn_D[J] note on diameter (1)meta.notecharn_LT[>=] remark on convergency of the Lyapunov Time (gravitational model) (2)meta.notecharLTLyapunov Time (gravitational model)yrtime.epochdoublen_LT0[>=] remark on convergency of the Lyapunov Time (Yarkovsky forces model, obliquity = 0 deg.) (3)meta.notecharLT0Lyapunov Time (Yarkovsky forces model, obliquity = 0 deg.)yrtime.epochdoublen_LT180[>=] remark on convergency of the Lyapunov Time (Yarkovsky forces model, obliquity = 180 deg.) (4)meta.notecharLT180Lyapunov Time (Yarkovsky forces model, obliquity = 180 deg.)yrtime.epochdoubledLT0Difference in Lyapunov Time values: LT0-LTyrtime.epoch;arith.diffdoubledLT180Difference in Lyapunov Time values: LT180-LTyrtime.epoch;arith.diffdouble