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Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis ofExpand
A large fraction of ~100 km class low-inclination objects in the classical Kuiper Belt (KB) are binaries with comparable masses and a wide separation of components. A favored model for theirExpand
Saturn's Small Inner Satellites: Clues to Their Origins
Cassini images of Saturn's small inner satellites have yielded their sizes, shapes, and in some cases, topographies and mean densities, and numerical N-body simulations of accretionary growth have provided clues to their internal structures and origins. Expand
Tidal Distortion and Disruption of Earth-Crossing Asteroids
Abstract We present results of numerical simulations that show that Earth's tidal forces can both distort and disrupt Earth-crossing asteroids that have weak “rubble-pile” structures. Building onExpand
Rotational breakup as the origin of small binary asteroids
It is found that mass shed from the equator of a critically spinning body accretes into a satellite if the material is collisionally dissipative and the primary maintains a low equatorial elongation. Expand
Direct Large-Scale N-Body Simulations of Planetesimal Dynamics
Abstract We describe a new direct numerical method for simulating planetesimal dynamics in which N ∼10 6 or more bodies can be evolved simultaneously in three spatial dimensions over hundreds ofExpand
Fragment properties at the catastrophic disruption threshold: The effect of the parent body’s internal structure
Abstract Numerical simulations of asteroid breakups, including both the fragmentation of the parent body and the gravitational interactions between the fragments, have allowed us to reproduceExpand
A Search for Jupiter-Mass Companions to Nearby Stars
Abstract We have carefully monitored the radial velocities of 21 bright, solar-type stars for 12 years, None has shown any reflex motion due to a substellar companion to an upper limit of between 1Expand
Collisions and Gravitational Reaccumulation: Forming Asteroid Families and Satellites
Results indicate that all large family members must be made of gravitationally reaccumulated fragments; that the post-collision member size distribution and the orbital dispersion are steeper and smaller, respectively, than for the evolved families observed today. Expand
Karin cluster formation by asteroid impact
Abstract Insights into collisional physics may be obtained by studying the asteroid belt, where large-scale collisions produced groups of asteroid fragments with similar orbits and spectra known asExpand