Broad-band laser interferometers are especially sensitive to the phase evolution of the gravitational
waves, which carry the information about the orbital phase evolution. The analysis of gravitational
wave data from such sources will involve some form of matched filtering of the noisy detector
output against an ensemble of theoretical “template” waveforms which depend on the intrinsic
parameters of the inspiralling binary, such as the component masses, spins, and so on, and on its
inspiral evolution. How accurate must a template be in order to “match” the waveform from a
given source (where by a match we mean maximizing the cross-correlation or the signal-to-noise
ratio)? In the total accumulated phase of the wave detected in the sensitive bandwidth, the
template must match the signal to a fraction of a cycle. For two inspiralling neutron stars, around
16,000 cycles should be detected during the final few minutes of inspiral; this implies a phasing
accuracy of 10^{–5} or better. Since v 1/10 during the late inspiral, this means that correction
terms in the phasing at the level of v^{5} or higher are needed. More formal analyses confirm this
intuition [67, 105, 68, 214].

Because it is a slow-motion system (v 10^{–3}), the binary pulsar is sensitive only to the lowest-order
effects of gravitational radiation as predicted by the quadrupole formula. Nevertheless, the first correction
terms of order v and v^{2} to the quadrupole formula were calculated as early as 1976 [268] (see
TEGP 10.3 [281]).

But for laser interferometric observations of gravitational waves, the bottom line is that, in order to measure the astrophysical parameters of the source and to test the properties of the gravitational waves, it is necessary to derive the gravitational waveform and the resulting radiation back-reaction on the orbit phasing at least to 2PN order beyond the quadrupole approximation, and preferably to 3PN order.

For the special case of non-spinning bodies moving on quasi-circular orbits (i.e. circular apart from a slow inspiral), the evolution of the gravitational wave frequency through 2PN order has the form

where . The first term is the quadrupole contribution (compare Equation (72)), the second term is the 1PN contribution, the third term, with the coefficient , is the “tail” contribution, and the fourth term is the 2PN contribution, first reported jointly by Blanchet et al. [40, 39, 291]. The 2.5PN, 3PN and 3.5PN contributions have also been calculated (see [34] for a review).Similar expressions can be derived for the loss of angular momentum and linear momentum. Expressions for non-circular orbits have also been derived [121, 75]. These losses react back on the orbit to circularize it and cause it to inspiral. The result is that the orbital phase (and consequently the gravitational wave phase) evolves non-linearly with time. It is the sensitivity of the broad-band laser interferometric detectors to phase that makes the higher-order contributions to so observationally relevant.

If the coefficients of each of the powers of in Equation (97) can be measured, then one again obtains more than two constraints on the two unknowns and , leading to the possibility to test GR. For example, Blanchet and Sathyaprakash [42, 41] have shown that, by observing a source with a sufficiently strong signal, an interesting test of the coefficient of the “tail” term could be performed.

Another possibility involves gravitational waves from a small mass orbiting and inspiralling into a (possibly supermassive) spinning black hole. A general non-circular, non-equatorial orbit will precess around the hole, both in periastron and in orbital plane, leading to a complex gravitational waveform that carries information about the non-spherical, strong-field spacetime around the hole. According to GR, this spacetime must be the Kerr spacetime of a rotating black hole, uniquely specified by its mass and angular momentum, and consequently, observation of the waves could test this fundamental hypothesis of GR [231, 213].

Thirdly, the dipole gravitational radiation predicted by scalar-tensor theories will result in a modification of the gravitational radiation back-reaction, and thereby of the phase evolution. Including only the leading quadrupole and dipole contributions, one obtains, in Brans–Dicke theory,

where , and is the coefficient of the dipole term, given by , where , , are given by Equations (94), and . Double neutron star systems are not promising because the small range of masses available near results in suppression of dipole radiation by symmetry. For black holes, s = 0.5 identically, consequently double black hole systems turn out to be observationally identical in the two theories. Thus mixed systems involving a neutron star and a black hole are preferred. However, a number of analyses of the capabilities of both ground-based and space-based (LISA) observatories have shown that observing waves from neutron-star–black-hole inspirals is not likely to bound scalar-tensor gravity at a level competitive with the Cassini bound or with future solar-system improvements [283, 161, 236, 292, 27, 28].http://www.livingreviews.org/lrr-2006-3 |
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