  Gravitational-wave memory refers to the permanent displacement of the test
masses in an idealized (freely-falling) gravitational-wave interferometer.
Inspiraling binaries produce a particularly interesting form of memory--the
Christodoulou memory. Although it originates from nonlinear interactions at 2.5
post-Newtonian order, the Christodoulou memory affects the gravitational-wave
amplitude at leading (Newtonian) order. Previous calculations have computed
this non-oscillatory amplitude correction during the inspiral phase of binary
coalescence. Using an "effective-one-body" description calibrated with the
results of numerical relativity simulations, the evolution of the memory during
the inspiral, merger, and ringdown phases, as well as the memory's final
saturation value, are calculated. Using this model for the memory, the
prospects for its detection are examined, particularly for supermassive black
hole binary coalescences that LISA will detect with high signal-to-noise
ratios. Coalescing binary black holes also experience center-of-mass recoil due
to the anisotropic emission of gravitational radiation. These recoils can
manifest themselves in the gravitational-wave signal in the form of a "linear"
memory and a Doppler shift of the quasi-normal-mode frequencies. The prospects
for observing these effects are also discussed.
