  We examine the main properties of gravitational waves (GWs) emitted by
transient hyperbolic encounters of black holes. We begin by building the set of
basic variables most relevant to setting our problem. After exposing the ranges
of masses and eccentricities accessible at a given GW frequency, we analyze the
dependence of the gravitational strain on those parameters and determine the
trajectories resulting in the most sizeable strains. Some non-trivial behaviors
are unveiled, showing that highly eccentric events can be more easily
detectable than parabolic ones. In particular, we underline the correct way to
extend formulas from hyperbolic to parabolic orbits. Our reasonings are as
general as possible, and we make a point of explaining our considerations
pedagogically.
