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#### Fast post-adiabatic waveforms in the time domain: Applications to compact binary coalescences in LIGO and Virgo

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2105.06983.pdf

(Preprint), 9MB

PhysRevD.104.124087.pdf

(Publisher version), 2MB

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##### Citation

Mihaylov, D., Ossokine, S., Buonanno, A., & Ghosh, A. (2021). Fast post-adiabatic
waveforms in the time domain: Applications to compact binary coalescences in LIGO and Virgo.* Physical
Review D,* *104*(12): 124087. doi:10.1103/PhysRevD.104.124087.

Cite as: https://hdl.handle.net/21.11116/0000-0008-8E15-1

##### Abstract

We present a computationally efficient (time-domain) multipolar waveform

model for quasi-circular spin-aligned compact binary coalescences. The model

combines the advantages of the numerical-relativity informed,

effective-one-body (EOB) family of models with a post-adiabatic solution of the

equations of motion for the inspiral part of the two-body dynamics. We

benchmark this model against other state-of-the-art waveforms in terms of

efficiency and accuracy. We find a speed-up of one to two orders of magnitude

compared to the underlying time-domain EOB model for the total mass range $2 -

100 M_{\odot}$. More specifically, for a low total-mass system, such as a

binary neutron star with equal masses of $1.4 M_{\odot}$, like GW170817, the

computational speedup is around 100 times; for an event with total mass $\sim

40 M_\odot$ and mass ratio $\sim 3$, like GW190412, the speedup is by a factor

of $\sim 20$, while for a binary system of comparable masses and total mass of

$\sim 70 M_{\odot}$, like GW150914, it is by a factor of $\sim 10$. We

demonstrate that the new model is extremely faithful to the underlying EOB

model with unfaithfulness less than $0.01\%$ across the entire applicable

region of parameter space. Finally, we present successful applications of this

new waveform model to parameter estimation studies and tests of general

relativity.

model for quasi-circular spin-aligned compact binary coalescences. The model

combines the advantages of the numerical-relativity informed,

effective-one-body (EOB) family of models with a post-adiabatic solution of the

equations of motion for the inspiral part of the two-body dynamics. We

benchmark this model against other state-of-the-art waveforms in terms of

efficiency and accuracy. We find a speed-up of one to two orders of magnitude

compared to the underlying time-domain EOB model for the total mass range $2 -

100 M_{\odot}$. More specifically, for a low total-mass system, such as a

binary neutron star with equal masses of $1.4 M_{\odot}$, like GW170817, the

computational speedup is around 100 times; for an event with total mass $\sim

40 M_\odot$ and mass ratio $\sim 3$, like GW190412, the speedup is by a factor

of $\sim 20$, while for a binary system of comparable masses and total mass of

$\sim 70 M_{\odot}$, like GW150914, it is by a factor of $\sim 10$. We

demonstrate that the new model is extremely faithful to the underlying EOB

model with unfaithfulness less than $0.01\%$ across the entire applicable

region of parameter space. Finally, we present successful applications of this

new waveform model to parameter estimation studies and tests of general

relativity.