First dynamical model for the (22) Kalliope's satellite

Details First dynamical model for the (22) Kalliope's satellite First dynamical model for the (22) Kalliope's satellite

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.3607v&link_type=abstract

American Astronomical Society, DPS meeting #35, #36.07; Bulletin of the American Astronomical Society, Vol. 35, p.1486

Physics

Optics

Scientific paper

The existence of binary asteroid systems was proven very recently from the space (Belton et al., Icarus, 1995) and from the ground with Adaptive Optics and Radar Observations (Merline et al., Asteroid III, 2003). Thought photometry, occultation observations, direct imaging (including Adaptative Optic and HST), radar methods and space probe, around 90 asteroids are suspected to be in fact a double system (see a list on http://www.imcce.fr/observateur/binast/binary_ast.php). Several questions about the stability of their orbit and their formation have been discussed and our group has been focusing on the moonlet system of 22 Kalliope.
We acquired 20 observations of the binary system between October 2001 and January 2003 using several Adaptive Optics systems (Lick, Palomar and VLT). We used the orbit characteristic derived by a geometrical model in Marchis et al., Icarus, 2003 as initial input. We used a dynamical model based on the 2-body problem perturbated by a zonal coefficient J2 to fit these observations. As the primary mass and the J2 are poorly known and as these parameters interact strongly in the model, it's difficult to find coherent results with all observations. Our first attempt is partially successful since we have fit in a coherent model the first 19 positions of Kalliope. We partially failed to predict the positions seen on the January 2003 images, even if the observed positions are located on the calculated orbit. We will give additional results considering several different masses and J2 coefficients. We will show that is necessary to include additional physical processes to improve our model. And finaly, additional observations (Margot and Brown, Science, 2003) may better constrain the density and distribution of mass of the primary to improve the model.

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