Asymptotic gravitational wave fluxes from a spinning particle in circular equatorial orbits around a rotating black hole

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F16%3A10335556" target="_blank" >RIV/00216208:11320/16:10335556 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1103/PhysRevD.93.044015" target="_blank" >http://dx.doi.org/10.1103/PhysRevD.93.044015</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevD.93.044015" target="_blank" >10.1103/PhysRevD.93.044015</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Asymptotic gravitational wave fluxes from a spinning particle in circular equatorial orbits around a rotating black hole

Popis výsledku v původním jazyce

We present a new computation of the asymptotic gravitational wave energy fluxes emitted by a spinning particle in circular equatorial orbits about a Kerr black hole. The particle dynamics is computed in the pole-dipole approximation, solving the Mathisson-Papapetrou equations with the Tulczyjew spin-supplementary-condition. The fluxes are computed, for the first time, by solving the 2 + 1 Teukolsky equation in the time-domain using hyperboloidal and horizon-penetrating coordinates. Denoting by M the black hole mass and by mu the particle mass, we cover dimensionless background spins a/M = (0, +/- 0.9) and dimensionless particle spins -0.9 <= S/mu(2) <= +0.9. Our results span orbits of Boyer-Lindquist coordinate radii 4 <= r/M <= 30; notably, we investigate the strong-field regime, in some cases even beyond the last-stable-orbit. We compare our numerical results for the gravitational wave fluxes with the 2.5th order accurate post-Newtonian (PN) prediction obtained analytically by Tanaka et al. [Phys. Rev. D 54, 3762 ( 1996)]: we find an unambiguous trend of the PN-prediction toward the numerical results when r is large. At r/M = 30 the fractional agreement between the full numerical flux, approximated as the sum over the modes m = 1, 2, 3, and the PN prediction is less than or similar to 0.5% in all cases tested. This is close to our fractional numerical accuracy (similar to 0.2%). For smaller radii, the agreement between the 2.5PN prediction and the numerical result progressively deteriorates, as expected. Our numerical data will be essential to develop suitably resummed expressions of PN-analytical fluxes in order to improve their accuracy in the strong-field regime.

Název v anglickém jazyce

Asymptotic gravitational wave fluxes from a spinning particle in circular equatorial orbits around a rotating black hole

Popis výsledku anglicky

We present a new computation of the asymptotic gravitational wave energy fluxes emitted by a spinning particle in circular equatorial orbits about a Kerr black hole. The particle dynamics is computed in the pole-dipole approximation, solving the Mathisson-Papapetrou equations with the Tulczyjew spin-supplementary-condition. The fluxes are computed, for the first time, by solving the 2 + 1 Teukolsky equation in the time-domain using hyperboloidal and horizon-penetrating coordinates. Denoting by M the black hole mass and by mu the particle mass, we cover dimensionless background spins a/M = (0, +/- 0.9) and dimensionless particle spins -0.9 <= S/mu(2) <= +0.9. Our results span orbits of Boyer-Lindquist coordinate radii 4 <= r/M <= 30; notably, we investigate the strong-field regime, in some cases even beyond the last-stable-orbit. We compare our numerical results for the gravitational wave fluxes with the 2.5th order accurate post-Newtonian (PN) prediction obtained analytically by Tanaka et al. [Phys. Rev. D 54, 3762 ( 1996)]: we find an unambiguous trend of the PN-prediction toward the numerical results when r is large. At r/M = 30 the fractional agreement between the full numerical flux, approximated as the sum over the modes m = 1, 2, 3, and the PN prediction is less than or similar to 0.5% in all cases tested. This is close to our fractional numerical accuracy (similar to 0.2%). For smaller radii, the agreement between the 2.5PN prediction and the numerical result progressively deteriorates, as expected. Our numerical data will be essential to develop suitably resummed expressions of PN-analytical fluxes in order to improve their accuracy in the strong-field regime.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BE - Teoretická fyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA14-10625S" target="_blank" >GA14-10625S: Obecně relativistická pole kompaktních astrofyzikálních zdrojů</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2016

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

—

Svazek periodika

93

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

22

Strana od-do

—

Kód UT WoS článku

000369437100004

EID výsledku v databázi Scopus

2-s2.0-84959493293