Fundamentally distinct outcomes of asteroid collisional evolution: Itokawa and Eros

Details Fundamentally distinct outcomes of asteroid collisional evolution: Itokawa and Eros Fundamentally distinct outcomes of asteroid collisional evolution: Itokawa and Eros

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007georl..3409201c&link_type=abstract

Geophysical Research Letters, Volume 34, Issue 9, CiteID L09201

Astronomy and Astrophysics

Astrophysics

4

Planetary Sciences: Comets And Small Bodies: Interiors (8147), Planetary Sciences: Comets And Small Bodies: Origin And Evolution, Planetary Sciences: Comets And Small Bodies: Surfaces, Planetary Sciences: Comets And Small Bodies: Impact Phenomena (5420, 8136), Planetary Sciences: Comets And Small Bodies: Instruments And Techniques

Scientific paper

The outcomes of asteroid collisional evolution are presently unclear: are most asteroids larger than 1 km size gravitational aggregates reaccreted from fragments of a parent body that was collisionally disrupted, while much smaller asteroids are collisional shards that were never completely disrupted? The 16 km mean diameter S-type asteroid 433 Eros, visited by the NEAR mission, has surface geology consistent with being a fractured shard. The Hayabusa spacecraft visited an S-asteroid smaller than 1 km, namely 25143 Itokawa. Here we report the first comparative analyses of Itokawa and Eros geology. Itokawa lacks a global lineament fabric, and its blocks, craters, and regolith are inconsistent with formation and evolution as a fractured shard, unlike Eros. Itokawa is not a scaled-down Eros, but formed by a distinct process of catastrophic disruption and reaccumulation.

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