From horseshoe to quasi-satellite and back again: the curious dynamics of Earth co-orbital asteroid 2015 SO2

Marcos, C. de la Fuente; Marcos, R. de la Fuente

doi:10.1007/s10509-015-2597-8

Cited by 9 publications

(2 citation statements)

References 36 publications

(54 reference statements)

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“…A very interesting case of mean motion resonance are the co-orbitals, that is, objects with the same orbital period or trapped in the resonance 1:1. There are several examples of co-orbitals in the solar system, and quasi-satellites are probably the most interesting [22]. They seem to be satellites of a planet but are just revolving around the Sun with the exact same planetary orbital period, sometimes ahead of the planet and sometimes behind, generating a relative trajectory with respect to the planet that seems to be a satellite-like orbit.…”

Section: Orbital Resonancesmentioning

confidence: 99%

Exploring the orbital evolution of planetary systems

Gallardo¹

2017

Eur. J. Phys.

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The aim of this paper is to encourage the use of orbital integrators in the classroom to discover and understand the long term dynamical evolution of systems of orbiting bodies. We show how to perform numerical simulations and how to handle output data in order to reveal the dynamical mechanisms that dominate the evolution of arbitrary planetary systems in timescales of millions of years using a simple but efficient numerical integrator. Through some examples we reveal the fundamental properties of planetary systems: the time evolution of the orbital elements, the free and forced modes that drive oscillations in eccentricity and inclination, the fundamental frequencies of the system, the role of the angular momenta, the invariable plane, orbital resonances, and the Kozai-Lidov mechanism.

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Section: Orbital Resonancesmentioning

confidence: 99%

Exploring the orbital evolution of planetary systems

Gallardo¹

2017

Eur. J. Phys.

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“…Spectroscopic analysis has shown that some members of this cluster exhibit a distinctive olivine-dominated composition that lends further support to the common origin scenario (Borisov et al 2017). On the E-mail: nbplanet@ucm.es other hand, most known Mars Trojans are believed to be primordial objects that may have remained in their current dynamical state since Mars was formed (Christou 2013;de la Fuente Marcos & de la Fuente Marcos 2013a;Christou et al 2017). The stability of Mars Trojans in general and of relevant known objects in particular has been studied by e.g.…”

Section: Introductionmentioning

confidence: 99%

Using Mars co-orbitals to estimate the importance of rotation-induced YORP break-up events in Earth co-orbital space

Marcos

2021

Monthly Notices of the Royal Astronomical Society

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Both Earth and Mars host populations of co-orbital minor bodies. A large number of present-day Mars co-orbitals is probably associated with the fission of the parent body of Mars Trojan 5261 Eureka (1990 MB) during a rotation-induced Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) break-up event. Here, we use the statistical distributions of the Tisserand parameter and the relative mean longitude of Mars co-orbitals with eccentricity below 0.2 to estimate the importance of rotation-induced YORP break-up events in Martian co-orbital space. Machine-learning techniques (k-means++ and agglomerative hierarchical clustering algorithms) are applied to assess our findings. Our statistical analysis identified three new Mars Trojans: 2009 SE, 2018 EC4, and 2018 FC4. Two of them, 2018 EC4 and 2018 FC4, are probably linked to Eureka but we argue that 2009 SE may have been captured, so it is not related to Eureka. We also suggest that 2020 VT1, a recent discovery, is a transient Martian co-orbital of the horseshoe type. When applied to Earth co-orbital candidates with eccentricity below 0.2, our approach led us to identify some clustering, perhaps linked to fission events. The cluster with most members could be associated with Earth quasi-satellite 469219 Kamo‘oalewa (2016 HO3) that is a fast rotator. Our statistical analysis identified two new Earth co-orbitals: 2020 PN1, which follows a horseshoe path, and 2020 PP1, a quasi-satellite that is dynamically similar to Kamo‘oalewa. For both Mars and Earth co-orbitals, we found pairs of objects whose values of the Tisserand parameter differ by very small amounts, perhaps hinting at recent disruption events. Clustering algorithms and numerical simulations both suggest that 2020 KZ2 and Kamo‘oalewa could be related.

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A trio of horseshoes: past, present and future dynamical evolution of Earth co-orbital asteroids 2015 XX 169 $\mbox{XX}_{169}$ , 2015 YA and 2015 YQ 1 $\mbox{YQ}_{1}$

Marcos¹,

Marcos²

2016

Astrophys Space Sci

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A trio of horseshoes: past, present and future dynamical evolution of Earth co-orbital asteroids 2015 XX 169 , 2015 YA and 2015 YQ 1 C. de la Fuente Marcos • R. de la Fuente Marcos Abstract It is widely accepted that a quasi-steadystate flux of minor bodies moving in and out of the co-orbital state with the Earth may exist. Some of these objects are very good candidates for future in situ study due to their favourable dynamical properties. In this paper, we show that the recently discovered nearEarth asteroids 2015 XX 169 , 2015 YA and 2015 YQ 1 are small transient Earth co-orbitals. These new findings increase the tally of known Earth co-orbitals to 17. The three of them currently exhibit asymmetric horseshoe behaviour subjected to a Kozai resonance and their short-term orbital evolution is rather unstable. Both 2015 YA and 2015 YQ 1 may leave Earth's co-orbital zone in the near future as they experience close encounters with Venus, the Earth-Moon system and Mars. Asteroid 2015 XX 169 may have remained in the vicinity of, or trapped inside, the 1:1 mean motion resonance with our planet for many thousands of years and may continue in that region for a significant amount of time into the future.

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From horseshoe to quasi-satellite and back again: the curious dynamics of Earth co-orbital asteroid 2015 SO2

Cited by 9 publications

References 36 publications

Exploring the orbital evolution of planetary systems

Exploring the orbital evolution of planetary systems

Using Mars co-orbitals to estimate the importance of rotation-induced YORP break-up events in Earth co-orbital space

A trio of horseshoes: past, present and future dynamical evolution of Earth co-orbital asteroids 2015 XX 169 $\mbox{XX}_{169}$ , 2015 YA and 2015 YQ 1 $\mbox{YQ}_{1}$

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