Collisional And Tidal Disruptions Of Small Solid Bodies: Influence Of The Internal Structure And Implications

Details Collisional And Tidal Disruptions Of Small Solid Bodies: Influence Of The Internal Structure And Implications Collisional And Tidal Disruptions Of Small Solid Bodies: Influence Of The Internal Structure And Implications

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6505m&link_type=abstract

American Astronomical Society, DPS meeting #38, #65.05; Bulletin of the American Astronomical Society, Vol. 38, p.615

Astronomy and Astrophysics

Astrophysics

Scientific paper

Although the theory of Roche for the tidal disruption limits of orbiting satellites assumes a fluid body, a length to diameter of exactly 2.07 :1, and a particular body orientation, the theory is commonly applied to the satellites of the Solar System and to small bodies passing nearby a planet, including Near-Earth Objects.
Numerical simulations of collisional disruptions of asteroids suggest that most planet-crossing bodies larger than a few hundreds of meters in size may well be gravitational aggregates or rubble piles. In particular, a large majority of NEOs originates from the main asteroid belt and these bodies are likely to be the fragments of larger ones that underwent a catastrophic impact. Most of these fragments consist of smaller ones that reaccumulated due to their gravitational interactions during the collisional process. Thus, such small bodies, consisting of gravitational aggregates, are neither fluids nor generally have a high degree of cohesion.
Here we recall the results of our simulations of collisions suggesting that a large majority of small bodies may well consist of rubble piles and we expose exact analytical results for the distortion and disruption limits of such solid spinning ellipsoidal bodies subjected to tidal forces. In particular, we will present the application of this theory to a few real objects, such as the asteroid 99942 Apophis (2004 MN4). Concerning this object, we checked whether its predicted distance to the Earth (5.6 +/- 1.4 Earth's radii) in 2029 is within the distance for which a tidal disruption or a shape adjustment may occur. For this, we assumed different values of its bulk density. We will then show that unless it is extremely porous (with a bulk density of only a few tenths of g/cm3), tidal readjustments are an extremely remote possibility.

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