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Communication Dans Un Congrès Année : 2010

Asteroid Pairs Formed by Rotational Fission

Résumé

A population of small main-belt asteroid pairs (MBAs) residing on very similar heliocentric orbits have been found and studied recently (Vokrouhlicky and Nesvorny, Astron. J. 136: 280 2008 and Astron. J. 137: 111 2009, Pravec and Vokrouhlicky, Icarus 204: 580 2009). These asteroid pairs show some common properties: they are ubiquitous with pairs found throughout the asteroid population, pair members are separated with low hyperbolic escape velocities (as low as 0.17 m/s), they are young with most pairs probably separated less than 1 Myr ago, and their sizes and mass ratios overlap with the population of orbiting, bound binary systems. Previous investigations of binary asteroids suggests that they were formed from parent bodies spinning at a critical rate by some sort of fission or mass shedding process (Pravec and Harris, Icarus 190: 250 2007, Scheeres, Icarus 189: 370 2007, Walsh et al., Nature 454: 188 2008), however the possibility that these two populations of asteroid pairs and binaries were related was intriguing but lacked of observational data.
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hal-03733926 , version 1 (21-07-2022)

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Daniel J. Scheeres, P. Pravec, D. Vokrouhlický, David Polishook, Alan W. Harris, et al.. Asteroid Pairs Formed by Rotational Fission. AAS/Division on Dynamical Astronomy Meeting #41, Apr 2010, Boston, Massachusetts, United States. pp.926. ⟨hal-03733926⟩
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