A population of Main Belt Asteroids co-orbiting with Ceres and Vesta

  title={A population of Main Belt Asteroids co-orbiting with Ceres and Vesta},
  author={Apostolos A. Christou and Paul A. Wiegert},
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 are
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 the
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 the
(309239) 2007 RW10: a large temporary quasi-satellite of Neptune
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
Resonances in the asteroid and trans–Neptunian belts: A brief review
  • T. Gallardo
  • Physics, Geology
    Planetary and Space Science
  • 2018
Analysis of the Karma asteroid family
The Karma asteroid family is a group of primitive asteroids in the middle part of the main belt, just at the outer edge of the 3J:1A mean-motion resonance. We obtained the list of the family members
Here we report on the significant role of a so far overlooked dynamical aspect, namely, a secular resonance between the dwarf planet Ceres and other asteroids. We demonstrate that this type of
Temporary capture of planetesimals by a giant planet and implication for the origin of irregular satellites
Performing global three-body orbital integration, we investigate temporary capture of planetesimals by a giant planet from their heliocentric orbits. We confirm four types of capture orbits, which
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 or


Co-orbital objects in the main asteroid belt
We have investigated the possibility of main belt as- teroids being trapped in the 1:1 resonance with other asteroids. Using contemporary mass estimates for the large asteroids (1) Ceres, (2) Pallas
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 computations
A Numerical Survey of Transient Co-orbitals of the Terrestrial Planets
Abstract We have investigated numerically the evolution of near-Earth asteroids (3753) Cruithne, (3362) Khufu, 1989 VA, (10563) 1993 WD, and 1994 TF2 that enter the coorbital regions of the Earth or
On the asteroid belt's orbital and size distribution
We have searched Microvariability and Oscillations of Stars (MOST) satellite photometry obtained in 2004, 2005, and 2007 of the solar-type star HD 209458 for Trojan asteroid swarms dynamically
An asteroidal companion to the Earth
Near-Earth asteroids range in size from a few metres to more than 30 km: in addition to playing an important role in past and present impact rates on the Earth, they might one day be exploited as
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 by
Asteroid Proper Elements and the Dynamical Structure of the Asteroid Main Belt
Abstract We have computed proper elements for 12,573 asteroids, including all the ones with orbits accurate enough to be useful for family identification. This was done with an upgraded version of
Dynamics of Mars Trojans
In this paper we explore the dynamical stability of the Mars Trojan region applying mainly Laskar’s Frequency Map Analysis. This yields the chaotic diffusion rate of orbits and allows to determine
S/2004 S 5 : A new co-orbital companion for Dione