Rubble Pile Asteroids

The moniker rubble pile is typically applied to all Solar System bodies >200 m and <∼10 km in diameter; in this size range, there is an abundance of evidence that nearly every object is bound primarily by self-gravity, with significant void space or bulk porosity between irregularly shaped con...

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Published in:Annual review of astronomy and astrophysics Vol. 56; no. 1; pp. 593 - 624
Main Author: Walsh, Kevin J
Format: Journal Article
Language:English
Published: Palo Alto Annual Reviews 14-09-2018
Annual Reviews, Inc
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Abstract The moniker rubble pile is typically applied to all Solar System bodies >200 m and <∼10 km in diameter; in this size range, there is an abundance of evidence that nearly every object is bound primarily by self-gravity, with significant void space or bulk porosity between irregularly shaped constituent particles. The understanding of this population is derived from wide-ranging population studies of derived shape and spin, decades of observational studies in numerous wavelengths, evidence left behind from impacts on planets and moons, and the in situ study of a few objects via spacecraft flyby or rendezvous. The internal structure, however, which is responsible for the name rubble pile, is never directly observed but belies a violent history. Many or most of the asteroids on near-Earth orbits and those most accessible for rendezvous and in situ study are likely by-products of the continued collisional evolution of the main asteroid belt.
AbstractList The moniker rubble pile is typically applied to all Solar System bodies >200 m and <∼10 km in diameter; in this size range, there is an abundance of evidence that nearly every object is bound primarily by self-gravity, with significant void space or bulk porosity between irregularly shaped constituent particles. The understanding of this population is derived from wide-ranging population studies of derived shape and spin, decades of observational studies in numerous wavelengths, evidence left behind from impacts on planets and moons, and the in situ study of a few objects via spacecraft flyby or rendezvous. The internal structure, however, which is responsible for the name rubble pile, is never directly observed but belies a violent history. Many or most of the asteroids on near-Earth orbits and those most accessible for rendezvous and in situ study are likely by-products of the continued collisional evolution of the main asteroid belt.
Author Walsh, Kevin J
AuthorAffiliation Southwest Research Institute, Boulder, Colorado 80302, USA; email
kwalsh@boulder.swri.edu
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  surname: Walsh
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Snippet The moniker rubble pile is typically applied to all Solar System bodies >200 m and <∼10 km in diameter; in this size range, there is an abundance of evidence...
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annualreviews
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SubjectTerms Asteroids
collisional evolution
Earth
Earth orbital rendezvous
Earth orbits
Evolution
Flyby missions
Observational studies
Orbits
Planets
Population studies
Porosity
rubble pile
Solar system
Solar System formation
Space rendezvous
Spacecraft
Void space
Wavelengths
Title Rubble Pile Asteroids
URI http://dx.doi.org/10.1146/annurev-astro-081817-052013
https://www.proquest.com/docview/2120894469
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