Adiabatic equatorial inspirals of a spinning body into a Kerr black hole

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00558962" target="_blank" >RIV/67985815:_____/22:00558962 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216208:11320/22:10446336

Výsledek na webu

<a href="https://doi.org/10.1103/PhysRevD.105.084033" target="_blank" >https://doi.org/10.1103/PhysRevD.105.084033</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevD.105.084033" target="_blank" >10.1103/PhysRevD.105.084033</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Adiabatic equatorial inspirals of a spinning body into a Kerr black hole

Popis výsledku v původním jazyce

The detection of gravitational waves from extreme mass ratio inspirals (EMRIs) by the future space based gravitational-wave detectors demands the generation of accurate enough waveform templates. Since the spin of the smaller secondary body cannot be neglected for the detection and parameter estimation of EMRIs, we study its influence on the phase of the gravitational waves from EMRIs with a spinning secondary. We focus on generic eccentric equatorial orbits around a Kerr black hole. To model the spinning secondary object, we use the Mathisson-Papapetrou-Dixon equations in the pole-dipole approximation. Furthermore, we linearize in spin the orbital variables and the gravitational-wave fluxes from the respective orbits. We obtain these fluxes by using the Teukolsky formalism in the frequency domain. We derive the evolution equations for the spin-induced corrections to the adiabatic evolution of an inspiral. Finally, through their numerical integration, we find the gravitational-wave phase shift between an inspiral of a spinning and a nonspinning body.

Název v anglickém jazyce

Adiabatic equatorial inspirals of a spinning body into a Kerr black hole

Popis výsledku anglicky

The detection of gravitational waves from extreme mass ratio inspirals (EMRIs) by the future space based gravitational-wave detectors demands the generation of accurate enough waveform templates. Since the spin of the smaller secondary body cannot be neglected for the detection and parameter estimation of EMRIs, we study its influence on the phase of the gravitational waves from EMRIs with a spinning secondary. We focus on generic eccentric equatorial orbits around a Kerr black hole. To model the spinning secondary object, we use the Mathisson-Papapetrou-Dixon equations in the pole-dipole approximation. Furthermore, we linearize in spin the orbital variables and the gravitational-wave fluxes from the respective orbits. We obtain these fluxes by using the Teukolsky formalism in the frequency domain. We derive the evolution equations for the spin-induced corrections to the adiabatic evolution of an inspiral. Finally, through their numerical integration, we find the gravitational-wave phase shift between an inspiral of a spinning and a nonspinning body.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/EF19_073%2F0016935" target="_blank" >EF19_073/0016935: Grantová schémata na UK</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

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

105

Číslo periodika v rámci svazku

8

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

23

Strana od-do

084033

Kód UT WoS článku

000807557100002

EID výsledku v databázi Scopus

2-s2.0-85129235255