In terms of the trace-reversed metric perturbation and in the Lorenz gauge in linearized gravity, the linearized Einstein equations on Minkowski spacetime are
For signature and the curvature convention giving , take , and . A trace-free Lorenz-gauge particular solution has the displayed form. The vector is null, and , so co-propagating test photons are undeflected by this beam field. For a transversely uniform source, is one particular solution. A function of alone has vanishing wave operator and cannot source nonzero ; homogeneous gravitational perturbations and boundary conditions remain separate data.
The retarded source solution of the Linearized Einstein equations is selected by excluding added incoming or freely specified homogeneous gravitational waves. A homogeneous wave can satisfy Lorenz gauge in linearized gravity while having no source mass quadrupole moment. Thus a formula for the retarded source field is not an identity for every solution of the sourced wave equation.
For a compact slowly moving source in the weak-field approximation, with no incoming homogeneous wave and , the retarded Linearized Einstein equations give this leading far-zone trace-reversed metric perturbation. The key consequence of stress-energy conservation is . The physical gravitational wave is obtained by the transverse-traceless projector.
Dropping the position-dependent source delay in the leading far-zone retarded field requires source size to be small compared with its variation time , in units . The retarded quadrupole field also requires . For a typical nonrelativistic bound source, implies this long-wavelength condition; an arbitrarily rapidly oscillating small displacement is not controlled merely by its instantaneous speed.
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