stars, modeled as point masses orbiting about each other in a circular orbit, induce a strain $s(t)$ at the detector given by $$s(t) = {\cal A} (\pi f(t) )^{2/3} \cos \left [\varphi (t) + \Phi\right],
\label {wave}$$ where $f(t)$ is the instantaneous gravitational wave frequency, the constant $\cal A$ involves the distance to the binary, its reduced and total mass, and the antenna pattern of the detector [@Th87] and $\Phi$ is the initial phase of the wave at some fiducial time $t=t_s$. The phase of the waveform $\varphi (t)$ contains several pieces corresponding to different post-Newtonian contributions which can be schematically written as $$\varphi(t) = \varphi_0(t) + \varphi_1(t) + \varphi_{1.5}(t) + \ldots.
\label {phase}$$ The evolution of the phase depends on the masses of the two components of the binary, characterised by the reduced mass, $\mu$ and the total mass, $M$ of the system. Here $\varphi_0(t)$ is the dominant Newtonian part of the phase and $\varphi_n(t)$ represents the $n$th order post-Newtonian correction to it. The Newtonian part of the phase is sensitive only to a particular combination of the masses of the two stars, frequently characterised by its ‘chirp mass’, ${\cal M} = \mu^{3/5}M^{2/5}$. We give below the waveform correct 