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 |
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Format: | Journal Article |
Language: | English |
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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. |
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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 |
AuthorAffiliation_xml | – name: Southwest Research Institute, Boulder, Colorado 80302, USA; email – name: kwalsh@boulder.swri.edu |
Author_xml | – sequence: 1 givenname: Kevin J surname: Walsh fullname: Walsh, Kevin J |
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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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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 |
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