Origin and dynamical evolution of the asteroid belt

Abstract

The asteroid belt was dynamically shaped during and after planet formation. Despite representing a broad ring of stable orbits, the belt contains less than one one-thousandth of an Earth mass. The asteroid orbits are dynamically excited with a wide range in eccentricity and inclination and their compositions are diverse, with a general trend toward dry objects in the inner belt and more water-rich objects in the outer belt. Here we review models of the asteroid belt's origins and dynamical history. The classical view is that the belt was born with several Earth masses in planetesimals, then strongly depleted. However, it is possible that very few planetesimals ever formed in the asteroid region and that the belt's story is one of implantation rather than depletion. A number of processes may have implanted asteroids from different regions of the Solar System, dynamically removed them, and excited their orbits. During the gaseous disk phase these include the effects of giant planet growth and migration and sweeping secular resonances. After the gaseous disk phase these include scattering from resident planetary embryos, chaos in the giant planets' orbits, the giant planet instability, and long-term dynamical evolution. Different global models for Solar System formation imply contrasting dynamical histories of the asteroid belt. Vesta and Ceres may have been implanted from opposite regions of the Solar System -- Ceres from the Jupiter-Saturn region and Vesta from the terrestrial planet region -- and could therefore represent very different formation conditions.

Chapter to appear in Vesta and Ceres: Insights into the Dawn of the Solar System (Cambridge U. Press; Editors Simone Marchi, Carol A. Raymond, and Christopher T. Russell). Updated figures

References in corpus (41)

• The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
• Protoplanetary Disk Structures in Ophiuchus
• Solar System evolution from compositional mapping of the asteroid belt
• Building Terrestrial Planets
• Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
• Dynamics of the giant planets of the solar system in the gaseous proto-planetary disk and relationship to the current orbital architecture
• The structure of protoplanetary discs around evolving young stars
• Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
• The Exoplanet Mass-Ratio Function from the MOA-II Survey: Discovery of a Break and Likely Peak at a Neptune Mass
• Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
• The timeline of the Lunar bombardment - revisited
• Highly Siderophile Elements in the Earth's Mantle as a Clock for the Moon-forming Impact
• Exotic Earths: Forming Habitable Worlds with Giant Planet Migration
• Close-in planetesimal formation by pile-up of drifting pebbles
• Initial mass function of planetesimals formed by the streaming instability
• Challenges in Planet Formation
• Constraints on resonant-trapping for two planets embedded in a protoplanetary disc
• Reduced gas accretion on super-Earths and ice giants
• Highly siderophile elements were stripped from Earth's mantle by iron sulfide segregation
• Lunar and Terrestrial Planet Formation in the Grand Tack Scenario
• The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
• Dynamical evidence for an early giant planet instability
• Short dissipation times of proto-planetary discs - an artifact of selection effects?
• On the formation of terrestrial planets in hot-Jupiter systems
• The Feeding Zones of Terrestrial Planets and Insights into Moon Formation
• Constraining the giant planets' initial configuration from their evolution: implications for the timing of the planetary instability
• Dynamical Shakeup of Planetary Systems II. N-body simulations of Solar System terrestrial planet formation induced by secular resonance sweeping
• Outward migration of Jupiter and Saturn in 3:2 or 2:1 resonance in radiative disks: implications for the Grand Tack and Nice models
• Terrestrial Planet Formation in the Presence of Migrating Super-earths
• Different origins or different evolutions? Decoding the spectral diversity among C-type asteroids
• The consequences of planetary migration on the minor bodies of the early Solar System
• Modeling the Historical Flux of Planetary Impactors
• Terrestrial Planet Formation from an Annulus
• Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?
• The Asteroid Belt as a Relic From a Chaotic Early Solar System
• The common origin of family and non-family asteroids
• Jovian Early Bombardment: planetesimal erosion in the inner asteroid belt
• A record of the final phase of giant planet migration fossilized in the asteroid belt's orbital structure
• Instabilities in the Early Solar System due to a Self-gravitating Disk
• On the inclinations of the Jupiter Trojans
• Scattering V-type asteroids during the giant planets instability: A step for Jupiter, a leap for basalt

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