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arXiv · 0712.0553

Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune

Harold F. Levison·Alessandro Morbidelli·Christa Van Laerhoven·Rodney Gomes·Kleomenis Tsiganis
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Abstract

We explore the origin and orbital evolution of the Kuiper belt in the framework of a recent model of the dynamical evolution of the giant planets, sometimes known as the Nice model. This model is characterized by a short, but violent, instability phase, during which the planets were on large eccentricity orbits. One characteristic of this model is that the proto-planetary disk must have been truncated at roughly 30 to 35 AU so that Neptune would stop migrating at its currently observed location. As a result, the Kuiper belt would have initially been empty. In this paper we present a new dynamical mechanism which can deliver objects from the region interior to ~35 AU to the Kuiper belt without excessive inclination excitation. Assuming that the last encounter with Uranus delivered Neptune onto a low-inclination orbit with a semi-major axis of ~27 AU and an eccentricity of ~0.3, and that subsequently Neptune's eccentricity damped in ~1 My, our simulations reproduce the main observed properties of the Kuiper belt at an unprecedented level.

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Harold F. Levison, Alessandro Morbidelli, Christa Van Laerhoven, Rodney Gomes, Kleomenis Tsiganis. 2007-12-04. Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune. https://doi.org/10.1016/j.icarus.2007.11.035

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