The third and a half post-Newtonian gravitational wave quadrupole mode for quasi-circular inspiralling compact binaries

Abstract

We compute the quadrupole mode of the gravitational waveform of inspiralling compact binaries at the third and a half post-Newtonian (3.5PN) approximation of general relativity. The computation is performed using the multipolar post-Newtonian formalism, and restricted to binaries without spins moving on quasi-circular orbits. The new inputs mainly include the 3.5PN terms in the mass quadrupole moment of the source, and the control of required subdominant corrections to the contributions of hereditary integrals (tails and non-linear memory effect). The result is given in the form of the quadrupolar mode (2,2) in a spin-weighted spherical harmonic decomposition of the waveform, and may be used for comparison with the counterpart quantity computed in numerical relativity. It is a step towards the computation of the full 3.5PN waveform, whose knowledge is expected to reduce the errors on the location parameters of the source.

19 pages, 1 figure; minor corrections, including some rephrasing in the introduction and in section IIIB

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Cited by in corpus (2)

• Improved effective-one-body description of coalescing nonspinning black-hole binaries and its numerical-relativity completion
• Spin effects on gravitational waves from inspiraling compact binaries at second post-Newtonian order