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Numerical simulations of the collisional disruption of large asteroids show that although the parent body is totally shattered, subsequent gravitational reaccumulation leads to the formation of an entire family of large and small objects with dynamical properties similar to those of the parent body. Simulations were performed in two different collisional(More)
In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier's archiving and manuscript policies are encouraged to visit: Abstract Evidence is mounting that asteroids larger than a few hundred metres in(More)
It has been suggested that asteroids between ~100 m and ~100 km in size may be gravita-tional aggregates of loosely consolidated material. Recently evidence has been mounting to support this idea. Comet breakups, crater chains, doublet craters, giant craters, grooves, asteroid spins, underdense asteroids, asteroid satellites, and unusual asteroid shapes can(More)
This paper builds on preliminary work in which numerical simulations of the collisional disruption of large asteroids (represented by the Eunomia and Koronis family parent bodies) were performed and which accounted not only for the fragmentation of the solid body through crack propagation, but also for the mutual gravita-tional interaction of the resulting(More)
standing of doublet craters, crater chains, and asteroids with peculiar shapes and spins. We present results of numerical simulations that show that asteroids that have weak ''rubble-pile'' structures. Building on previous studies, we consider more realistic asteroid shapes and trajectories, test a variety of spin rates and axis orientations, 1.(More)
A tree code method that incorporates a local shearing disc model and fourth-order integration algorithm is applied to the problem of planetary rings, with particular emphasis on the dynamics of Saturn's B ring. The new code, described in detail elsewhere, allows for particle self-gravity, a distribution of particle sizes, and surface friction (particle(More)
Asteroid families are groups of small bodies that share certain orbit and spectral properties. More than 20 families have now been identified, each believed to have resulted from the collisional break-up of a large parent body in a regime where gravity controls the outcome of the collision more than the material strength of the rock. The size and velocity(More)
We present numerical experiments investigating the shape and spin limits of self-gravitating " perfect " rubble piles that consist of identical, smooth, rigid, spherical particles with configurable normal coefficient of restitution and no sliding friction. Such constructs are currently employed in a variety of investigations, ranging from the formation of(More)
Cassini images of Saturn's small inner satellites (radii of less than approximately 100 kilometers) have yielded their sizes, shapes, and in some cases, topographies and mean densities. This information and numerical N-body simulations of accretionary growth have provided clues to their internal structures and origins. The innermost ring-region satellites(More)