Abstract
In studies of orbital dynamics of celestial bodies it is also usually possible to explain chaotic manifestations by using paradigmatic models of interaction and overlap of non-linear resonances, addressed in the first part of the book. In this chapter, we consider major classes of the Solar system minor bodies on the subject of their actual or potential chaotic behaviour. These classes include: planetary satellite systems (in particular, the Miranda–Umbriel, Mimas–Tethys, and Prometheus–Pandora systems); near-Earth asteroids (NEAs), main-belt asteroids and Kuiper belt objects; and comets, which are typically highly chaotic. In connection with the considered dynamical populations, concepts of two-body and three-body resonances and secular resonances are considered. Dynamical environments of small bodies, and, in particular, chaotic zones around contact binaries (such as famous KBO 2014 MU69), are analytically characterized.
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