Gravitational Aggregates: Evidence and Evolution

By Derek C. Richardson, Z. Leinhardt, H. Melosh, E. Asphaug. 2002

211 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a9d612c8db3259a4257f280700b09969bbbc1be6

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Citations in the corpus

The global effects of impact-induced seismic activity on fractured asteroid surface morphology (2005, background): “Further work has characterized an entire spectrum of asteroid structural types, called 'gravitational aggregates' by Richardson et al. (2002), which span the extremes from monolith to highly comminuted rubble pile.”
Gravitational N-Body Simulations (2003, background): “A review of the properties of such gravitational aggregates is also available [Richardson et al., 2003].”
Rubble Pile Asteroids (2018, background): “While this community-wide effort to clarify the properties of small bodies in Richardson et al. (2002) specified a name of “gravitational aggregate” for low-strength and high porosity objects, the terminology of “rubble pile” remained in common use, and fully returned to prominence with the…”
Spin-up of rubble-pile asteroids: Disruption, satellite formation, and equilibrium shapes (2012, methodology): “Such bodies are also commonly called rubble piles or gravitational aggregates (see Richardson et al., 2002 for a detailed discussion and definition of gravitational aggregates).”
The hazard of near-Earth asteroid impacts on earth (2004, background): “most asteroids, including those of sub-kilometer sizes, should be rubble piles or at least battered and badly fractured [42].”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, background): “If kilometer-sized asteroids are predominantly gravitational aggregates (or, as many call them, rubble-pile asteroids; Richardson et al. 2002), or they are as weak as suggested by strength models (Holsapple 2005), YORP may spin some of them up so fast that they change shape, shed mass, or even…”
The fossilized size distribution of the main asteroid belt (2003, methodology): “D smooth particle hyd dynamics (SPH) code(Benz and Asphaug, 1999)combined with theN -body code pkdgrav(Richardson et al. 2002; Leinhardt et al., 2000; Leinhardt and Richards 2002).”
Effects of thermal radiation on the dynamics of binary NEAs (2004, background): “The fast rotation and regular shape of most primaries have usually been ascribed to their being “rubble piles” spinning close to the rotational disruption limit (Richardson et al., 2002).”
The formation of asteroid satellites in large impacts: Results from numerical simulations (2004, background): “Conceptually, however, the largest remnants are bodies that have been completely shattered and reassembled, a special case of a gravitational aggregate fitting one definition of a rubble pile (see Richardson et al., 2002, for a review).”
Asteroid Density, Porosity, and Structure (2002, background): “Those with low macroporosity are solid, coherent objects, while high macroporosities values indicate loosely consolidated objects that may be collections of rubble held together by gravity (see Richardson et al., 2002).”
Formation of Phobos and Deimos via a giant impact (2015, unknown): “E P] 1 9 M ar 2 01 5”