A low density of 0.8 g cm-3 for the Trojan binary asteroid 617 Patroclus

@article{Marchis2006ALD,
  title={A low density of 0.8 g cm-3 for the Trojan binary asteroid 617 Patroclus},
  author={Franck Marchis and Daniel Hestroffer and Pascal Descamps and J{\'e}r{\^o}me Berthier and Antonin H. Bouchez and Randall D. Campbell and Jason C. Y. Chin and Marcos A. van Dam and Scott K. Hartman and Erik M. Johansson and Robert Lafon and David Le Mignant and Imke de Pater and Paul J. Stomski and Douglas M. Summers and Fr{\'e}d{\'e}ric Vachier and Peter L. Wizinovich and Michael H. Wong},
  journal={Nature},
  year={2006},
  volume={439},
  pages={565-567}
}
The Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and located at the L4 and L5 stable Lagrange points of the Jupiter–Sun system (leading and following Jupiter by 60°). The asteroid 617 Patroclus is the only known binary Trojan. The orbit of this double system was hitherto unknown. Here we report that the components, separated by 680 km, move around the system's centre of mass, describing a roughly circular orbit. Using this orbital information… 
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References

SHOWING 1-10 OF 33 REFERENCES
Chaotic capture of Jupiter's Trojan asteroids in the early Solar System
TLDR
It is shown that the Trojans could have formed in more distant regions and been subsequently captured into co-orbital motion with Jupiter during the time when the giant planets migrated by removing neighbouring planetesimals.
Discovery of the triple asteroidal system 87 Sylvia
TLDR
The unambiguous detection of a triple asteroidal system in the main belt, composed of a 280-km primary (87 Sylvia) and two small moonlets orbiting at 710 and 1,360 km, which was most probably formed through the disruptive collision of a parent asteroid.
The Albedo Distribution of Jovian Trojan Asteroids
We present radiometrically derived V-band geometric albedos and effective radii for 32 Jovian Trojan asteroids, using near-simultaneous mid-infrared and visible observations. We sampled the large end
Eclipsing binary asteroid 90 Antiope
CCD observations of the binary asteroid 90 Antiope were carried out at seven observatories (Borowiec, Kharkiv, Pic du Midi, Chateau Renard, Les Engarouines, Ottmarsheim, and Durtal) on 31 nights from
Discovery of a moon orbiting the asteroid 45 Eugenia
Evidence for asteroidal satellites (moons) has been sought for decades, because the relative frequency of such satellites will bear on the collisional history of the asteroid belt and the Solar
The binary Kuiper-belt object 1998 WW31
TLDR
It is reported that the Kuiper-belt object 1998 WW31 is binary with a highly eccentric orbit (eccentricity e ≈ 0.8) and a long period (about 570 days), very different from the Pluto/Charon system, which was hitherto the only previously known binary in theKuiper belt.
Formation of Kuiper-belt binaries by dynamical friction and three-body encounters
TLDR
It is shown that a transient binary forms when two large bodies penetrate one another's Hill sphere (the region where their mutual forces are larger than the tidal force of the Sun) and the loss of energy needed to stabilize the binary orbit can occur through dynamical friction from surrounding small bodies, or through the gravitational scattering of a third large body.
Amalthea's Density Is Less Than That of Water
TLDR
It is suggested that Amalthea is porous and composed of water ice, as well as rocky material, and thus formed in a cold region of the solar system, possibly not at its present location near Jupiter.
...
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