The Dynamical Structure of the Kuiper Belt and its Primordial Origin
arXiv:astro-ph/0703558
Abstract
This chapter discusses the dynamical properties of the Kuiper belt population. Then, it focuses on the characteristics of the Kuiper belt that cannot be explained by its evolution in the framework of the current solar system. We review models of primordial solar system evolution that have been proposed to reproduce the Kuiper belt features, outlining advantages and problems of each of them.
arXiv commentto be published in `Transneptunian Objects', Barucci et al. eds., University of Arizona Press
References in corpus (16)
- Catastrophic disruptions revisited
- Planetesimal Formation by Gravitational Instability
- Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
- Photoevaporation of Circumstellar Disks due to External FUV Radiation in Stellar Aggregates
- Orbital Evolution of Planets Embedded in a Planetesimal Disk
- Planet Formation by Coagulation: A Focus on Uranus and Neptune
- Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12
- Evidence for early stellar encounters in the orbital distribution of Edgeworth-Kuiper Belt objects
- On the Size-Dependence of the Inclination Distribution of the Main Kuiper Belt
- The Size Distribution of Kuiper Belt Objects
- Stellar encounters as the origin of distant solar system objects in highly eccentric orbits
- The Edge of the Solar System
- The Effects of a Stellar Encounter on a Planetesimal Disk
- Accretion in the Early Outer Solar System
- Diverse Albedos of Small Trans-Neptunian Objects
- On the AU Mic debris disk: density profiles, grain properties and dust dynamics