SÉMINAIRE DU GRECO
"4.5 PostNewtonian order gravitational radiation" 

Tanguy Marchand 

PostNewtonian theory enables us to predict the waveform of the gravitational waves emitted by a system of two compact objects coalescing in its inspiral phase. Stateoftheart works provide the phase of the expected signal up to 3.5PN (i.e. up to 1/c^7). Comparison with numerical relativity, as well as the promising evolution of gravitational wave detectors incite us to pursue this computation to a higher order. In our current project, we are aiming at reaching phase of the signal at the 4.5PN order (i.e. 1/c^9). For this purpose, the flux emitted by such a system has to be known at 4.5PN. One difficulty of this computation is the highorder interactions  commonly called tails between the mass of the system and its mass and current multipole moments during the propagation of the signal. After a broad introduction to BlanchetDamourIyer formalism used to perform our computation, I will show how the work done in [1], has enabled us to determine the 4.5PN coefficient of the flux (while the 4PN coefficient is still unknown).


lundi 27 février 2017  11:00 Salle des séminaires Évry Schatzman, Institut d'Astrophysique de Paris 
