Comparing second-order gravitational self-force, numerical relativity, and effective one body waveforms from inspiralling, quasicircular, and nonspinning black hole binaries

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00564726" target="_blank" >RIV/67985815:_____/22:00564726 - isvavai.cz</a>

Alternative codes found

RIV/00216208:11320/22:10457108

Result on the web

<a href="https://doi.org/10.1103/PhysRevD.106.084061" target="_blank" >https://doi.org/10.1103/PhysRevD.106.084061</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevD.106.084061" target="_blank" >10.1103/PhysRevD.106.084061</a>

Result language

angličtina

Original language name

Comparing second-order gravitational self-force, numerical relativity, and effective one body waveforms from inspiralling, quasicircular, and nonspinning black hole binaries

Original language description

We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasicircular and nonspinning black hole binaries computed with three different approaches: second-order gravitational self-force (2GSF) theory, as implemented in the 1PAT1 model, numerical relativity (NR), as implemented by the SXS collaboration, and the effective one body (EOB) formalism, as implemented in the TEOBRESUMS waveform model. To compare the models we use both a standard, time-domain waveform alignment and a gauge-invariant analysis based on the dimensionless function Qw(w)w2/_w, where w is the gravitational wave frequency. We analyze the domain of validity of the 1PAT1 model, deriving error estimates and showing that the effects of the final transition to plunge, which the model neglects, extend over a significantly larger frequency interval than one might expect. Restricting to the inspiral regime, we find that, while for mass ratios q = m1/m2 <= 10 TEOBRESUMS is largely indistinguishable from NR, 1PAT1 has a significant dephasing N1 rad, conversely, for q N 100, 1PAT1 is estimated to have phase errors < 0.1 rad on a large frequency interval, while TEOBRESUMS develops phase differences N1 rad with it. Most crucially, on that same large frequency interval we find good agreement between TEOBRESUMS and 1PAT1 in the intermediate regime 15 < q < 64, with < 0.5 rad dephasing between them. A simple modification to the TEOBRESUMS flux further improves this agreement for q N 30, reducing the dephasing to approximate to 0.27 rad even at q = 128. While our analysis points to the need for more highly accurate, long-inspiral, NR simulations for q N 15 to precisely quantify the accuracy of EOB/2GSF waveforms, we can clearly identify the primary sources of error and routes to improvement of each model. In particular, our results pave the way for the construction of GSF-informed EOB models for both intermediate and extreme mass ratio inspirals for the next generation of gravitational wave detectors.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

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Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2022

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Physical Review D

ISSN

2470-0010

e-ISSN

2470-0029

Volume of the periodical

106

Issue of the periodical within the volume

8

Country of publishing house

US - UNITED STATES

Number of pages

32

Pages from-to

084061

UT code for WoS article

000880793000014

EID of the result in the Scopus database

2-s2.0-85141564188