Coorbital Dynamics at Large Eccentricity and Inclination

Namouni, Fathi; Christou, Apostolos; Murray, C. D.

doi:10.1103/physrevlett.83.2506

Cited by 84 publications

(81 citation statements)

References 19 publications

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“…(or singularities) of this potential (Namouni, 1999;Namouni et al, 1999). Since the orbital elements vary in time, the shape of the averaged disturbing function changes as well.…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

“…He also numerically integrated the equations of motion in the circular restricted three-body problem for arbitrary values of the eccentricity and inclination of the asteroid's orbit. Namouni et al (1999) discussed the theory of the motion in the 1 : 1 resonance for large eccentricity and high inclination. Nesvorný et al (2002) developed such a theory in the planar elliptic three-body problem.…”

Section: Theory Of Co-orbital Motion For Arbitrary Eccentricities Andmentioning

confidence: 99%

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2002 AA29: Earth's recurrent quasi-satellite?

Wajer¹

2009

Icarus

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We study the dynamical evolution of asteroid 2002 AA 29 . This object moves in the co-orbital region of the Earth and is the first known asteroid which experiences We distinguish a few moments in time crucial for understanding its dynamics. Near 2400 and 2500 this object will be close to going through the maxima of the averaged disturbing function and it will either change its co-orbital regime by transition from the HS into QS state, or leave the librating mode. These approaches generate instability in the motion of 2002 AA 29 . By means of 66 observations, covering a two-year interval, we extend the analysis of the long term evolution of this object presented by Connors et al. (2002) and Brasser et al. (2004a). Our analysis is based on a sample of 100 cloned orbits. We show that the motion of 2002 AA 29 is predictable in the time interval [−2600, 7100] and outside of this interval the past and future orbital history can be studied using statistical methods.

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“…(or singularities) of this potential (Namouni, 1999;Namouni et al, 1999). Since the orbital elements vary in time, the shape of the averaged disturbing function changes as well.…”

Section: Accepted M Manuscriptmentioning

confidence: 99%

Section: Theory Of Co-orbital Motion For Arbitrary Eccentricities Andmentioning

confidence: 99%

2002 AA29: Earth's recurrent quasi-satellite?

Wajer¹

2009

Icarus

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“…The regularity breaks down if the object remains close to the planet or in the vicinity of the separatrix (Namouni, 1999;Namouni et al, 1999).…”

Section: Accepted Manuscriptmentioning

confidence: 99%

“…Quasi-satellites move outside of the planet's Hill sphere at the mean distance from the associated planet of the order of O(e), where e is the eccentricity of the object. For sufficiently large values of eccentricity and/or high enough inclination transitions between QS and HS (or TP) orbits are possible, and there can exist compound orbits which are unions of the HS (or TP) and QS orbits (Namouni, 1999;Namouni et al, 1999;Christou, 2000;Brasser et al, 2004a) So far quasi-satellites have been found for Venus, Earth and Jupiter. Venus currently has one temporary quasi-satellite object 2002 VE 68 and also one compound HS-QS orbiter (Brasser et al, 2004a).…”

Section: Introductionmentioning

confidence: 99%

Dynamical evolution of Earth’s quasi-satellites: 2004 GU9 and 2006 FV35

Wajer

2010

Icarus

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“…For a L 4 Trojan the libration is around +60 • , for a L 5 Trojan the libration is around −60 • or 300 • (see e.g. Murray & Dermott 1999), although the oscillation centre could be significantly shifted from the typical equilateral location in the case of eccentric orbits (Namouni, Christou & Murray 1999;Namouni & Murray 2000). The current value of λ r for 2014 YX 49 is ∼61 • , which suggests that 2014 YX 49 could be indeed a present-day Uranian Trojan, but this must be confirmed using N-body simulations (for 2011 QF 99 , a Trojan, is ∼47 • and ∼170 • for 472651, a horseshoe librator).…”

Section: Introductionmentioning

confidence: 99%

Asteroid 2014 YX$_\mathbf {49}$: a large transient Trojan of Uranus

Marcos¹,

Marcos²

2017

Mon. Not. R. Astron. Soc.

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In the outer Solar system, primordial Trojan asteroids may have remained dynamically stable for billions of years. • 83), is larger (absolute magnitude of 8.5 versus 9.7) and its libration period is slightly shorter (5.1 versus 5.9 kyr); contrary to 2011 QF 99 , its discovery was not the result of a targeted survey. It is less stable than 2011 QF 99 ; our extensive N-body simulations show that 2014 YX 49 may have been following a tadpole trajectory ahead of Uranus for about 60 kyr and it can continue doing so for another 80 kyr. Our analysis suggests that it may remain as co-orbital for nearly 1 Myr. As in the case of 2011 QF 99 , the long-term stability of 2014 YX 49 is controlled by Jupiter and Neptune, but it is currently trapped in the 7:20 mean motion resonance with Saturn. Consistently, the dynamical mechanism leading to the capture into and the ejection from the Trojan state involves ephemeral multibody mean motion resonances.

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Coorbital Dynamics at Large Eccentricity and Inclination

Cited by 84 publications

References 19 publications

2002 AA29: Earth's recurrent quasi-satellite?

2002 AA29: Earth's recurrent quasi-satellite?

Dynamical evolution of Earth’s quasi-satellites: 2004 GU9 and 2006 FV35

Asteroid 2014 YX$_\mathbf {49}$: a large transient Trojan of Uranus

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