Origin of the structure of the Kuiper belt during a dynamical instability in the orbits of Uranus and Neptune
H LEVISON et al. (2008)
- Published
- Jul 1, 2008
- Journal
- Icarus · Vol. 196 · No. 1
- DOI
- 10.1016/j.icarus.2007.11.035
At a GlanceAI
Links Kuiper belt structure to Uranus–Neptune orbital instability, explaining resonant and excited populations in a unified scenario.
SummaryAI
The work connects the observed orbital structure of Kuiper belt objects to a brief dynamical instability involving Uranus and Neptune, rather than to smooth, slow planet migration alone. By tying resonant trapping and the excitation of Kuiper belt orbits to an instability episode, it offers a coherent explanation for why multiple Kuiper belt sub-populations (including mean-motion resonances) look the way they do today. This frames Kuiper belt resonances as fossil records of the giant planets’ past rearrangement. The implication is that interpreting Kuiper belt resonant populations requires modeling the outer planets’ potentially chaotic early evolution.
Method SnapshotAI
Dynamical modeling of outer-planet orbital evolution and its effects on Kuiper belt object orbits, focusing on resonance capture and excitation.
BackgroundAI
Celestial mechanics of mean-motion resonances and basic Solar System dynamics, especially giant-planet migration/instability scenarios.