Orateur
Description
Compact binaries are the primary sources of gravitational waves, and an accurate description of their dynamics is essential for constructing waveform templates for future gravitational-wave detectors. Recently, the gravitational radiation-reaction force for non-spinning compact binaries on generic orbits has been derived in harmonic coordinates at the fourth-and-a-half post-Newtonian (4.5PN) order of general relativity.
Using this result, together with the Keplerian parametrization of the motion and Lagrange's method of variation of constants, I will present the computation of the corresponding radiation-reaction corrections to eccentric quasi-elliptic and quasi-hyperbolic orbits of two compact bodies at 4.5PN order.
This requires consistently incorporating the nonlocal-in-time tail contributions arising at 4PN order, together with the gravitational-wave recoil in the center-of-mass frame at 4.5PN order. I will also discuss how the results for bound and unbound orbits are explicitly related through analytic continuation.
| Which working group does your abstract concern? | Formes d'ondes / Waveforms |
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