Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune

@article{Levison2008OriginOT,
  title={Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune},
  author={Harold F. Levison and Alessandro Morbidelli and Christa L. Van Laerhoven and Rodney Gomes and Kleomenis Tsiganis},
  journal={Icarus},
  year={2008},
  volume={196},
  pages={258-273}
}
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384 Citations
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384 Citations

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References

SHOWING 1-10 OF 98 REFERENCES
The origin of Pluto's orbit: implications for the
The origin of the highly eccentric, inclined, and resonance-locked orbit of Pluto has long been a puzzle. A possible explanation has been proposed recently which suggests that these extraordinary…
Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna)
Explaining the origin of the orbits of 2000 CR105 (a = 230 AU, q = 44 AU) and 2003 VB12 (a = 531 AU, q = 74 AU, unofficially known as Sedna) is a major test for our understanding of the primordial…
The origin of the Kuiper Belt high-inclination population
SCENARIOS FOR THE ORIGIN OF THE ORBITS OF THE TRANS-NEPTUNIAN OBJECTS 2000 CR 105 AND 2003 VB 12 ( SEDNA )
Explaining the origin of the orbits of 2000 CR105 (a 1⁄4 230 AU, q 1⁄4 44 AU) and 2003 VB12 (a 1⁄4 531 AU, q 1⁄4 74 AU, unofficially known as Sedna) is a major test for our understanding of the…
Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets
TLDR
This model not only naturally explains the Late Heavy Bombardment, but also reproduces the observational constraints of the outer Solar System.
Embedded star clusters and the formation of the Oort Cloud
The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk
The Orbital and Spatial Distribution of the Kuiper Belt
Models of the evolution of Neptune’s migration and the dynamical processes at work during the formation of the outer solar system can be constrained by measuring the orbital distribution of the…
Orbital Evolution of Planets Embedded in a Planetesimal Disk
The existence of the Oort comet cloud, the Kuiper belt, and plausible inefficiencies in planetary core formation all suggest that there was once a residual planetesimal disk of mass ~10–100 M⊕ in the…
Origin of the orbital architecture of the giant planets of the Solar System
TLDR
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.
...
...