Satellites of asteroids have been discovered in nearly every known small body
population, and a remarkable aspect of the known satellites is the diversity of
their properties. They tell a story of vast differences in formation and
evolution mechanisms that act as a function of size, distance from the Sun, and
the properties of their nebular environment at the beginning of Solar System
history and their dynamical environment over the next 4.5 Gyr. The mere
existence of these systems provides a laboratory to study numerous types of
physical processes acting on asteroids and their dynamics provide a valuable
probe of their physical properties otherwise possible only with spacecraft.
Advances in understanding the formation and evolution of binary systems have
been assisted by: 1) the growing catalog of known systems, increasing from 33
to nearly 250 between the Merline et al. (2002) Asteroids III chapter and now,
2) the detailed study and long-term monitoring of individual systems such as
1999 KW4 and 1996 FG3, 3) the discovery of new binary system morphologies and
triple systems, 4) and the discovery of unbound systems that appear to be
end-states of binary dynamical evolutionary paths.
Specifically for small bodies (diameter smaller than 10 km), these
observations and discoveries have motivated theoretical work finding that
thermal forces can efficiently drive the rotational disruption of small
asteroids. Long-term monitoring has allowed studies to constrain the system's
dynamical evolution by the combination of tides, thermal forces and rigid body
physics. The outliers and split pairs have pushed the theoretical work to
explore a wide range of evolutionary end-states.Comment: 42 pages, 4 figures, contribution to the Asteroids 4 boo