(309239) 2007 RW10: a large temporary quasi-satellite of Neptune

@article{Marcos20123092392R,
  title={(309239) 2007 RW10: a large temporary quasi-satellite of Neptune},
  author={C. D. L. F. Marcos and R. D. L. F. Marcos},
  journal={Astronomy and Astrophysics},
  year={2012},
  volume={545}
}
Upon discovery, asteroid (309239) 2007 RW10 was considered a Neptune Trojan candidate. The object is currently listed by the Minor Planet Center as a Centaur but it is classified as a Scattered Disk or Trans-Neptunian Object by others. Now that its arc-length is 8,154 days and has been observed for more than 20 years, a more robust classification should be possible. Here we explore the orbital behaviour of this object in order to reveal its current dynamical status; we perform N-body… Expand
15 Citations

Figures and Tables from this paper

Plutino (15810) 1994 JR1, an accidental quasi-satellite of Pluto
In the Solar system, quasi-satellites move in a 1:1 mean motion resonance going around their host body like a retrograde satellite but their mutual separation is well beyond the Hill radius and theExpand
Crantor, a short-lived horseshoe companion to Uranus
Context. Stable co-orbital motion with Uranus is vulnerable to planetary migration, but temporary co-orbitals may exist today. So far, only two candidates have been suggested, both moving onExpand
Asteroid (469219) 2016 HO3, the smallest and closest Earth quasi-satellite
A number of Earth co-orbital asteroids experience repeated transitions between the quasi-satellite and horseshoe dynamical states. Asteroids 2001 GO2, 2002 AA29, 2003 YN107 and 2015 SO2 areExpand
A carefully characterised trans-neptunian survey
The Trans-Neptunian Objects (TNOs) preserve evidence of planet building processes in their orbital and size distributions. While all populations show steep size distributions for large objects,Expand
Four temporary Neptune co-orbitals: (148975) 2001 XA255, (310071) 2010 KR59, (316179) 2010 EN65, and 2012 GX17
Numerical simulations suggest that Neptune primordial co-orbitals may outnumber the equivalent population hosted by Jupiter, yet the objects remain elusive. Since the first discovery in 2001 just 10Expand
Transient Jupiter Co-orbitals from Solar System Sources
We demonstrate dynamical pathways from main-belt asteroid and Centaur orbits to those in co-orbital motion with Jupiter, including the retrograde (inclination $i>90^o$) state. We estimate that at anyExpand
A Uranian Trojan and the Frequency of Temporary Giant-Planet Co-Orbitals
TLDR
The detection of a Uranian Trojan is reported and a Centaur model is constructed, supplied from the transneptunian region, to estimate temporary co-orbital capture frequency and duration, finding that at any time 0.4 and 2.8% of the population will be Uranian and Neptunian co-orbitals, respectively. Expand
Asteroid 2014 OL339: yet another Earth quasi-satellite
Our planet has one permanently bound satellite -the Moon-, a likely large number of mini-moons or transient irregular natural satellites, and three temporary natural retrograde satellites orExpand
Comparative orbital evolution of transient Uranian co-orbitals: exploring the role of ephemeral multibody mean motion resonances
Uranus has three known co-orbitals: 83982 Crantor (2002 GO9), 2010 EU65 and 2011 QF99. Here, we perform a comparative analysis of the orbital evolution of these transient co-orbitals to understandExpand
The analemma criterion: accidental quasi-satellites are indeed true quasi-satellites
In the Solar system, a quasi-satellite is an object that follows a heliocentric path with an orbital period that matches almost exactly with that of a host body (planetary or not). The trajectory isExpand
...
1
2
...

References

SHOWING 1-10 OF 29 REFERENCES
On the dynamical evolution of 2002 VE68
The minor planet 2002 VE68 was identified as a quasi-satellite of Venus shortly after its discovery. At that time its data-arc span was only 24 d; now it is 2947 d. Here we revisit the topic of theExpand
Asteroid 2002 VE68, a quasi-satellite of Venus
The asteroid 2002 VE68 is currently a quasi-satellite of Venus, the first object of this dynamical class to be discovered, and is also the first known co-orbital companion to Venus. Our computationsExpand
2004 KV18: a visitor from the scattered disc to the Neptune Trojan population
We have performed a detailed dynamical study of the recently identified Neptunian Trojan 2004 KV18, only the second object to be discovered librating around Neptune's trailing Lagrange point, L5. WeExpand
The dynamics of Neptune Trojans – II. Eccentric orbits and observed objects
In a previous paper, we presented a global view of the stability of Neptune Trojans (NTs hereafter) on inclined orbits. As the continuation of the investigation, we discuss in this paper theExpand
A long-lived horseshoe companion to the Earth
We present a dynamical investigation of a newly found asteroid, 2010 SO 16, and the discovery that it is a horseshoe companion of the Earth. The object's absolute magnitude (H = 20.7) makes this theExpand
Origin and dynamical evolution of Neptune Trojans – II. Long-term evolution
Following our earlier work studying the formation of the Neptunian Trojan population during the planet's migration, we present results examining the eventual fate of the Trojan clouds produced inExpand
Transient co-orbital asteroids
Abstract We analyze the orbital behavior of four new co-orbital NEOs and the Earth horseshoe object 2002 AA29. The new objects are 2001 CK32, a 3753 Cruithne-like co-orbital of Venus, 2001 GO2 andExpand
The Orbital Evolution of Near-Earth Asteroid 3753
Asteroid 3753 (1986 TO) is in a 1:1 mean motion resonance with Earth, on a complex horseshoe-type orbit. Numerical experiments are performed to determine its medium-term stability and the means byExpand
A population of Main Belt Asteroids co-orbiting with Ceres and Vesta
Abstract We have carried out a search for Main Belt Asteroids (MBAs) co-orbiting with the large MBA Vesta and the dwarf planet Ceres. Through improving the search criteria used in Christou (Christou,Expand
THE RESONANT TRANS-NEPTUNIAN POPULATIONS*
The trans-Neptunian objects (TNOs) trapped in mean-motion resonances with Neptune were likely emplaced there during planet migration late in the giant-planet formation process. We perform detailedExpand
...
1
2
3
...