  We compute the gravitational waveform from a binary system in scalar-tensor
gravity at 2PN relative order. We restrict our calculation to non-spinning
binary systems on quasi-circular orbits and compute the spin-weighted spherical
modes of the radiation. The evolution of the phase of the waveform is computed
in the time and frequency domains. The emission of dipolar radiation is the
lowest-order dissipative process in scalar-tensor gravity. However, stringent
constraints set by current astrophysical observations indicate that this effect
is subdominant to quadrupolar radiation for most prospective gravitational-wave
sources. We compute the waveform for systems whose inspiral is driven by: (a)
dipolar radiation (e.g., binary pulsars or spontaneously scalarized systems)
and (b) quadrupolar radiation (e.g., typical sources for space-based and
ground-based detectors).
