Steins Properties in Comparison with Those of the Other Asteroids Visited by Space Missions

Details Steins Properties in Comparison with Those of the Other Asteroids Visited by Space Missions Steins Properties in Comparison with Those of the Other Asteroids Visited by Space Missions

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusm.p12a..07f&link_type=abstract

American Geophysical Union, Spring Meeting 2009, abstract #P12A-07

Astronomy and Astrophysics

Astrophysics

6040 Origin And Evolution, 6055 Surfaces, 6094 Instruments And Techniques, 6099 General Or Miscellaneous, 6205 Asteroids

Scientific paper

Rosetta spacecraft flown-by the asteroid Steins of September 5th, 2008 exploring for the first time an E type asteroid. The onboard camera OSIRIS, the visible and infrared spectroimager VIRTIS, the ultraviolet spectrometer ALICE, and the microwave spectrometer MIRO collected an important set of data which allows us to characterize the asteroid. As indicated by its meteorite analogues (the aubrites), the material believed to compose Steins is highly differentiated: the asteroid is a remnant of a large body destroyed by a chatastrophic collision. The surface morphology, dominated by several "fresh" craters, implies that the disruption of the Steins' parent body is relatively recent. The Steins' diamond shape is the consequence of the YORP effect. A comparative analysis of the properties of Gaspra, Ida, Eros, Mathilde, Itokawa and Steins provides some important hints for the understanding of the evolution of the solar system through the physical, chemical, and dynamical history of the asteroid population.

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