Detailed Pictures of Multiple Asteroid Systems in the Main-Belt

Details Detailed Pictures of Multiple Asteroid Systems in the Main-Belt Detailed Pictures of Multiple Asteroid Systems in the Main-Belt

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21e..07m&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #P21E-07

Physics

Optics

[5494] Planetary Sciences: Solid Surface Planets / Instruments And Techniques, [6035] Planetary Sciences: Comets And Small Bodies / Orbital And Rotational Dynamics, [6040] Planetary Sciences: Comets And Small Bodies / Origin And Evolution, [6024] Planetary Sciences: Comets And Small Bodies / Interiors

Scientific paper

Since their discovery less than 10 years ago, ~200 known multiple asteroid systems have been studied with a combination of observing techniques, including adaptive optics, lightcurve photometry, and mid-infrared spectrophotometry. Those observations show that ~15 large (D>100km) asteroids that are known to possess km-sized satellite(s) (22 Kalliope, 45 Eugenia, 87 Sylvia, 93 Minerva, 216 Kleopatra, ...) share common orbital characteristics, implying a common formation scenario: e.g. catastrophic disruption or ejection after an oblique impact. More than 70 smaller (10-15km) binary asteroid systems have been detected through anomalies in their lightcurves and are believed to have formed by fission due to the YORP effect. By comparison with meteorite analog densities, mid-IR data reveal that these systems have a significant porosity (larger than 30%) implying a rubble-pile interior. We will review these key results and discuss their implications for the interior of asteroids in the light of recent space mission results. Future explorations using new ground-based facilities and space mission concepts will be also discussed. This work is supported by the NSF grant AAG-0807468 and NASA grant NNX11AD62G

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