J/A+A/686/A107ivo://CDS.VizieR/J/A+A/686/A107doi:10.26093/cds/vizier.36860107CDSKovacova M.2024-11-29T20:02:38Z2024-06-03T09:25:44ZCDS support team

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

cds-question@unistra.frsolar-systemasteroidsResonances in the main asteroid belt play a significant role in the dynamical evolution of small bodies. They are capable of driving objects into the near-Earth object (NEO) region as well. This work re-examines the transportation abilities of the 5:2 mean motion resonance (MMR) with Jupiter. We focus on a greater portion of the resonance than the previous study that used a similar method. We are also interested in an elimination course along q~0.26au that was discovered previously. Moreover, we search for the orbits of potentially hazardous asteroids (PHAs) have and for orbits that correspond to recent L chondrite meteorites. Firstly, short-term fast Lyapunov indicator maps of the 5:2 MMR were computed in order to distinguish between stable and unstable orbits. Then over 10000 unstable particles were selected and integrated for a longer period of time, up to 10Myr, to reveal the transportation abilities of the resonance. During our simulation, 99.45% of test particles became NEOs, 9.43% reached the orbit with a semi-major axis, a<1au, and over 27% of particles migrated to low perihelion distances q<0.005au. In addition, 92.8% of the particles entered the Hill sphere of the Earth and over 97% reached an orbit at which we would classify them as potentially hazardous if they were sufficiently large. However, our simulation did not confirm ejections along q~0.26au. Our results suggest that there is some kind of discrepancy between using the MERCURIUS integrator (REBOUND package) and the ORBIT9 integrator (OrbFit package). This subject is worth additional examination.2024A&A...686A.107Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/686/A107CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/astorb : Orbits of Minor Planets (Bowell+, 2014-)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/686/A107https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/686/A107http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/686/A107https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/686/A107https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/686/A107http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/686/A107GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/686/A107/table3Total number and percentage of test particles that recovered the orbits of PHAs and orbital elements of PHAsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPlanet? Asteroid number of PHAmeta.numberintnullableNameName of PHAmeta.idcharDesignPreliminary designation PHA between bracketsmeta.id;meta.maincharNTotal number of test particles recovering the orbit of PHAmeta.numberintNfracFraction of test particles recovering the orbit of PHA%meta.numberfloataSemi-major axis (for epoch JD 2460200.5) (1)AUphys.size.smajAxisfloateEccentricity (JD 2460200.5) (1)src.orbital.eccentricityfloatiInclination (JD 2460200.5) (1)degsrc.orbital.inclinationfloatomegaArgument of perihelion (JD 2460200.5) (1)degsrc.orbital.periastronfloatOmegaLongitude of ascending node (JD 2460200.5) (1)degsrc.orbital.nodefloat