The Dynamics of NEO Binary Asteroids (original) (raw)
2007, Proceedings of the International Astronomical Union
The dynamics of binary asteroids in the Near Earth Object (NEO) space are discussed and constraints on their evolution presented. The dynamics of binary NEO involve coupling between their rotational states and the orbital dynamics of the system to an extent not found elsewhere in the current solar system. Due to this close coupling classical approximations that can be used for the dynamics of planetary satellites no longer apply and force more general considerations. In addition, due to the small total mass of these binary systems they are susceptible to external perturbations from the sun, planetary flybys, and even from solar irradiation via the YORP effect. Also, the evolutionary dynamics of these systems depend on the poorly understood mechanisms by which granular material aggregates dissipate energy. Despite these complexities, several basic rules governing the evolution of binary asteroid systems can be established and their implications considered in light of the observed state of binary asteroid systems. These also lead to competing theories of binary asteroid formation and subsequent evolution that still require formal validation. These theories primarily involve the balance between planetary flybys and solar irradiation effects on these small systems, although the solar tide can also become significant for some systems. We explore the implications of each of these perturbation sources and their possible effect on NEO binary systems, along with possible signatures that they could leave on these systems as they form and evolve.
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