A Thick Cloud of Neptune Trojans and Their Colors

  title={A Thick Cloud of Neptune Trojans and Their Colors},
  author={Scott S. Sheppard and Chadwick A. Trujillo},
  pages={511 - 514}
The dynamical and physical properties of asteroids offer one of the few constraints on the formation, evolution, and migration of the giant planets. Trojan asteroids share a planet's semimajor axis but lead or follow it by about 60° near the two triangular Lagrangian points of gravitational equilibrium. Here we report the discovery of a high-inclination Neptune Trojan, 2005 TN53. This discovery demonstrates that the Neptune Trojan population occupies a thick disk, which is indicative of “freeze… 
The capture of Trojan asteroids by the giant planets during planetary migration
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We present the results of detailed dynamical simulations of the effect of the migration of the four giant planets on both the transport of pre-formed Neptune Trojans and the capture of new Trojans
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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 in


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Abstract We present analytic and numerical results which illustrate the effects of Jupiter's accretion of nebular gas and the planet's radial migration on its Trojan companions. Initially, we
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The problem of accretion in the Trojan 1 : 1 resonance is akin to the standard problem of planet formation, transplanted from a star-centered disk to a disk centered on the Lagrange point. The newly
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The hypothesis of planetary migration is tested by numerically integrating orbits of Trojan-type asteroids in the gravitational field of the Sun, the migrating parent planet, and at least one extra
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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.
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Abstract Numerical and analytical calculations demonstrate that small planetesimals exhibit long-term stability of libration about the L4 and L5 Lagrange equilibrium points at a proto-Jupiter's
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It is shown that the objects currently observed in the dynamically cold Kuiper belt were most probably formed within ∼35 au and were subsequently pushed outward by Neptune's 1:2 mean motion resonance during its final phase of migration.
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This model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations, provided that Jupiter and Saturn crossed their 1:2 orbital resonance.