Dynamics and kinematics of celestial bodies and systems

The existing and new equipment will be used to observe small solar system bodies and double and multiple stars. The observations will be reduced, analyzed and submitted to the international data centers. Theoretical studies will include new classification of asteroids into families and the subsequent analyses of identified families, studies of the chaotic diffusion and non gravitational effects, as well as the development of tools for these studies. Extension to extrasolar systems will be attempted to investigate the small-body populations in different planetary configurations. Improved methods to compute orbits of double and multiple stars, in particular from the short arcs, will be developed, as well as the procedure to compute orbit grades. Masses, parallaxes and absolute magnitudes of the components will be determined for the Main-Sequence stars, and the physical characteristics will be studied in more detail for the systems for which relative coordinates, radial velocities and light curves are available. Unbiased samples of stars will be formed to study the local kinematics. The separation of stars and star clusters belonging to different subsystems and the study of the relations between the kinematical parameters and the stellar metallicity will be performed. Improved proper motions of Hipparcos stars will be determined from the long series of ground based observations and used to extend the reference system to the near infrared domain.