S E M I N A R IDepartament d'Astronomia i Astrofísica
Universitat de València
Coalescing binary black holes in the extreme mass ratio limit: comparison between analytical and numerical results
Relativity and Gravitation Group, Politecnico di Torino, Itàlia
Seminari del departament d'Astronomia i Astrofísica
Dijous 19 octubre 2006
Using black hole perturbation theory and Post-Newtonian resummation techniques for the radiation-reaction force, we determine the gravitational wave signature for the transition inspiral-plunge-ringdown for a binary (non-spinning) black hole system in the extreme mass ratio. We discuss energy, angular momentum and linear momentum losses and focus on the mechanism of excitation of the black hole Quasi-Normal-Modes. We propose analytical methods, based on Effective-One-Body ideas, to reproduce the smooth transition between the inspiral and the ringdown phase of the gravitational waveform. We show that the it is possible to build an analytical "effective" waveform whose phase differs of less than 1% per cycle with respect to the actual signal. Implication for the equal mass black hole case and gravitational wave detection are briefly discussed.