Comparing second-order gravitational self-force and effective-one-body waveforms from inspiralling, quasicircular black hole binaries with a nonspinning primary and a spinning secondary

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00597856" target="_blank" >RIV/67985815:_____/24:00597856 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216208:11320/24:10484325

Výsledek na webu

<a href="https://doi.org/10.1103/PhysRevD.110.044034" target="_blank" >https://doi.org/10.1103/PhysRevD.110.044034</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevD.110.044034" target="_blank" >10.1103/PhysRevD.110.044034</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Comparing second-order gravitational self-force and effective-one-body waveforms from inspiralling, quasicircular black hole binaries with a nonspinning primary and a spinning secondary

Popis výsledku v původním jazyce

We present the first comparison of waveforms evaluated using the effective-one-body (EOB) approach and gravitational self-force (GSF) theory for inspiralling black hole binaries with a nonspinning primary and a spinning secondary. This paper belongs to a series of papers comparing the EOB model TEOBResumS esum S to GSF results, where the latter are used to benchmark the EOB analytical choices in the large-mass-ratio regime. In this work, we explore the performance of two gauge choices for the gyro-gravitomagnetic functions G(S), G(S) entering the spin-orbit sector within the EOB dynamics. In particular, we consider the usual gauge of TEOBResumS, esum S, where G(S) and G(S) only depend on the inverse radius and the radial momentum, and a different gauge where these functions also depend on the azimuthal momentum. The latter choice allows us to exploit as prefactor in G(S), the complete expression G(S*)(K) for a spinning particle on Kerr. As done previously, we employ both waveform alignments in the time domain and a gauge-invariant frequency- domain analysis to gain a more complete understanding of the impact of the new analytical choice. The frequency-domain analysis is particularly useful in confirming that the gyro-gravitomagnetic functions in the new chosen gauge bring the EOB spin contribution at first postadiabatic order closer to the GSF one. We finally implement the improved functions within the public code for TEOBResum S-Dali, which already incorporates eccentricity. In this way, we upgrade the EOB model for extreme-mass-ratio inspirals presented in our previous work.

Název v anglickém jazyce

Comparing second-order gravitational self-force and effective-one-body waveforms from inspiralling, quasicircular black hole binaries with a nonspinning primary and a spinning secondary

Popis výsledku anglicky

We present the first comparison of waveforms evaluated using the effective-one-body (EOB) approach and gravitational self-force (GSF) theory for inspiralling black hole binaries with a nonspinning primary and a spinning secondary. This paper belongs to a series of papers comparing the EOB model TEOBResumS esum S to GSF results, where the latter are used to benchmark the EOB analytical choices in the large-mass-ratio regime. In this work, we explore the performance of two gauge choices for the gyro-gravitomagnetic functions G(S), G(S) entering the spin-orbit sector within the EOB dynamics. In particular, we consider the usual gauge of TEOBResumS, esum S, where G(S) and G(S) only depend on the inverse radius and the radial momentum, and a different gauge where these functions also depend on the azimuthal momentum. The latter choice allows us to exploit as prefactor in G(S), the complete expression G(S*)(K) for a spinning particle on Kerr. As done previously, we employ both waveform alignments in the time domain and a gauge-invariant frequency- domain analysis to gain a more complete understanding of the impact of the new analytical choice. The frequency-domain analysis is particularly useful in confirming that the gyro-gravitomagnetic functions in the new chosen gauge bring the EOB spin contribution at first postadiabatic order closer to the GSF one. We finally implement the improved functions within the public code for TEOBResum S-Dali, which already incorporates eccentricity. In this way, we upgrade the EOB model for extreme-mass-ratio inspirals presented in our previous work.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2024

Kód důvěrnosti údajů

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

Název periodika

Physical Review D

ISSN

2470-0010

e-ISSN

2470-0029

Svazek periodika

110

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

16

Strana od-do

044034

Kód UT WoS článku

001294893000005

EID výsledku v databázi Scopus

2-s2.0-85201673772