The third post-Newtonian gravitational wave polarizations and associated spherical harmonic modes for inspiralling compact binaries in quasi-circular orbits

By L. Blanchet, G. Faye, B. Iyer, Siddhartha Sinha. 2008

207 citations recorded by the source corpus.

The gravitational waveform (GWF) generated by inspiralling compact binaries moving in quasi-circular orbits is computed at the third post-Newtonian (3PN) approximation to general relativity. Our motivation is two-fold: (i) to provide accurate templates for the data analysis of gravitational wave inspiral signals in laser interferometric detectors; (ii) to provide the associated spin-weighted spherical harmonic decomposition to facilitate comparison and match of the high post-Newtonian prediction for the inspiral waveform to the numerically-generated waveforms for the merger and ringdown. This extension of the GWF by half a PN order (with respect to previous work at 2.5PN order) is based on the algorithm of the multipolar post-Minkowskian formalism, and mandates the computation of the relations between the radiative, canonical and source multipole moments for general sources at 3PN order. We also obtain the 3PN extension of the source multipole moments in the case of compact binaries, and compute the contributions of hereditary terms (tails, tails-of-tails and memory integrals) up to 3PN order. The end results are given for both the complete plus and cross polarizations and the separate spin-weighted spherical harmonic modes.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/4d675ba0dffbbcb301236878a441c8b350c9250c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Geophysics

Citations in the corpus

Black-hole binaries, gravitational waves, and numerical relativity (2010, background): “Decades of work in this area have already been covered (Blanchet, 2006, 2010; Blanchet et al., 2008; Damour and Nagar, 2010; Schäfer, 2010).”
The Effective Field Theorist's Approach to Gravitational Dynamics (2016, unknown): “;kl Z+1 1 d! 2ˇ h !2ei!t ren()ei tail(!;) (1 + G NMj!jˇ) i Iij src(!); (7.86) hTT ij J-tail (tren;x) = 2GN r ij;kl Z+1 1 d! 2ˇ h !2ei!t ren()ei’ tail(!;) (1 + G NMj!jˇ) i Jij src(!); (7.87) with [78,174{176,178,179] tail(!;) GNM! log !2 ˇ2 + E 11 6 ; ’tail(!;) GNM! log !2 ˇ2 + E 7 3 : (7.88) The”
Surrogate model of hybridized numerical relativity binary black hole waveforms (2018, background): “The spherical harmonic modes of the PN waveform can be written (after rescaling to unit total mass and unit distance) as [74,82]”
Binary Black Hole Mergers in the First Advanced LIGO Observing Run (2016, methodology): “We use models of the waveform covering the inspiral, merger, and ringdown phases based on combining post-Newtonian (PN) theory [19–24], the effective-onebody (EOB) formalism [25–29], and numerical relativity simulations [30–36].”