New analytic representation of the ringdown waveform of coalescing spinning black hole binaries

@article{Damour2014NewAR,
  title={New analytic representation of the ringdown waveform of coalescing spinning black hole binaries},
  author={T. Damour and Alessandro Nagar},
  journal={Physical Review D},
  year={2014},
  volume={90},
  pages={024054}
}
We propose a new way of analyzing, and analytically representing, the ringdown part of the gravitational wave signal emitted by coalescing black hole binaries.By contrast with the usual {\it linear} decomposition of the multipolar complex waveform $h(t)$ in a sum of quasi-normal modes, our procedure relies on a {\it multiplicative} decomposition of $h(t)$ as the product of the fundamental quasi-normal mode with a remaining time-dependent complex factor whose amplitude and phase are separately… 

Figures and Tables from this paper

Enriching the symphony of gravitational waves from binary black holes by tuning higher harmonics

For the first time, we construct an inspiral-merger-ringdown waveform model within the effective-one-body formalism for spinning, nonprecessing binary black holes that includes gravitational modes

Multipolar effective one body waveform model for spin-aligned black hole binaries

We introduce {\tt TEOBiResumS_SM}, an improved version of the effective-one-body (EOB) waveform model {\tt TEOBResumS} for spin-aligned, coalescing black hole binaries, that includes subdominant

Effective-one-body waveforms from dynamical captures in black hole binaries

Dynamical capture is a possible formation channel for BBH mergers leading to highly eccentric merger dynamics and to gravitational wave (GW) signals that are morphologically different from those of

Modeling ringdown II: non-precessing binary black holes

The aftermath of binary black hole coalescence is a perturbed remnant whose gravitational radiation rings down, encoding information about the new black hole's recent history and current state. It is

Efficient effective one body time-domain gravitational waveforms

Computationally efficient waveforms are of central importance for gravitational wave data analysis of inspiralling and coalescing compact binaries. We show that the post-adiabatic (PA) approximation

Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors

We improve the accuracy of the effective-one-body (EOB) waveforms that were employed during the first observing run of Advanced LIGO for binaries of spinning, nonprecessing black holes by calibrating

Multipolar effective one body model for nonspinning black hole binaries

We introduce TEOBiResumMultipoles, a nonspinning inspiral-merger-ringdown waveform model built within the effective-one-body (EOB) framework that includes gravitational waveform modes beyond the

Comparison of various methods to extract ringdown frequency from gravitational wave data

The ringdown part of gravitational waves in the final stage of merger of compact objects tells us the nature of strong gravity which can be used for testing the theories of gravity. The ringdown

Machine learning gravitational waves from binary black hole mergers

We apply machine learning methods to build a time-domain model for gravitational waveforms from binary black hole mergers, called mlgw. The dimensionality of the problem is handled by representing

Towards the routine use of subdominant harmonics in gravitational-wave inference: Reanalysis of GW190412 with generation X waveform models

We re-analyse the gravitational-wave event GW190412 with state-of-the-art phenomenological waveform models. This event, which has been associated with a black hole merger, is interesting due to the

References

SHOWING 1-10 OF 24 REFERENCES

“A and B”:

Direct fabrication of large micropatterned single crystals. p1205 21 Feb 2003. (news): Academy plucks best biophysicists from a sea of mediocrity. p994 14 Feb 2003.

A and V

Phys

  • Rev. D76, 064028
  • 2007

Phys

  • Rev. D79, 064004
  • 2009

and C

  • Reisswig, Phys.Rev.Lett. 108, 131101
  • 2012

Phys

  • Rev. D64, 124013
  • 2001

and L

  • Rezzolla, Phys.Rev. D77, 084017
  • 2008

Phys

  • Rev. D 89, 084006
  • 2014

Phys

  • Rev. D62, 084011
  • 2000

Phys

  • Rev.D74, 104005
  • 2006