The Structure of the Distant Kuiper Belt in a Nice Model Scenario

Abstract

This work explores the orbital distribution of minor bodies in the outer Solar System emplaced as a result of a Nice model migration from the simulations of Brasser & Morbidelli (2013). This planetary migration scatters a planetesimal disk from between 29-34 AU and emplaces a population of objects into the Kuiper belt region. From the 2:1 Neptune resonance and outward, the test particles analyzed populate the outer resonances with orbital distributions consistent with trans-Neptunian object (TNO) detections in semi-major axis, inclination, and eccentricity, while capture into the closest resonances is too efficient. The relative populations of the simulated scattering objects and resonant objects in the 3:1 and 4:1 resonances are also consistent with observed populations based on debiased TNO surveys, but the 5:1 resonance is severely underpopulated compared to population estimates from survey results. Scattering emplacement results in the expected orbital distribution for the majority of the TNO populations, however the origin of the large observed population in the 5:1 resonance remains unexplained.

15 pages, 5 figures

References in corpus (5)

• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Sedna and the Oort Cloud Around a Migrating Sun
• The History of the Solar System's Debris Disc: Observable Properties of the Kuiper Belt
• A Possible Divot in the Size Distribution of the Kuiper Belt's Scattering Objects
• The 5:1 Neptune Resonance as Probed by CFEPS: Dynamics and Population

Cited by in corpus (8)

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• Is There an Earth-like Planet in the Distant Kuiper Belt?
• Can the orbital distribution of Neptune's 3:2 mean motion resonance result from stability sculpting?
• Calibration of the angular momenta of the minor planets in the solar system
• A study of the high-inclination population in the Kuiper belt -- IV. High-order mean motion resonances in the classical region
• The Surfaces of Small to Mid-Size Plutinos: Evidence of an Association Between Inclination and Surface Type