  (Abridged) In this celebratory contribution, we present some new data from
standard star cluster modelling containing primordial binaries and triples, as
well as results from a binary black hole simulation with two massive members.
In the star cluster case, the process of mass loss from evolving stars,
together with general mass segregation, promotes favourable interactions
involving compact subsystems of binaries and triples in the central region.
Three-body interactions often lead to energetic ejections, with one or more of
the components attaining relatively large terminal velocities which can be
observed in principle. The second type of stellar system to be discussed is
based on the scenario of two approaching galactic cores with density cusps,
each having a massive black hole. After the subsystems become well mixed, the
two massive components soon form a hard binary which gains energy by ejecting
other members. Such a massive binary has a large cross section and can be very
effective in depleting bound stars from the core. Again high-velocity escapers
are produced, with their terminal speeds related to the shrinking binary size
which eventually leads to coalescence.
