Eccentric binary black holes: Comparing numerical relativity and small mass-ratio perturbation theory
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Eccentric binary black holes : Comparing numerical relativity and small mass-ratio perturbation theory. / Ramos-Buades, Antoni; Meent, Maarten van de; Pfeiffer, Harald P.; Rueter, Hannes R.; Scheel, Mark A.; Boyle, Michael; Kidder, Lawrence E.
I: Physical Review D, Bind 106, Nr. 12, 124040, 28.12.2022.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Eccentric binary black holes
T2 - Comparing numerical relativity and small mass-ratio perturbation theory
AU - Ramos-Buades, Antoni
AU - Meent, Maarten van de
AU - Pfeiffer, Harald P.
AU - Rueter, Hannes R.
AU - Scheel, Mark A.
AU - Boyle, Michael
AU - Kidder, Lawrence E.
PY - 2022/12/28
Y1 - 2022/12/28
N2 - The modeling of unequal mass binary black hole systems is of high importance to detect and estimate parameters from these systems. Numerical relativity (NR) is well suited to study systems with comparable component masses, m1 similar to m2, whereas small mass ratio (SMR) perturbation theory applies to binaries where q = m2/m1 MUCH LESS-THAN 1. This work investigates the applicability for NR and SMR as a function of mass ratio for eccentric nonspinning binary black holes. We produce 52 NR simulations with mass ratios between 1:10 and 1:1 and initial eccentricities up to 0.8. From these we extract quantities like gravitational wave energy and angular momentum fluxes and periastron advance, and assess their accuracy. To facilitate comparison, we develop tools to map between NR and SMR inspiral evolutions of eccentric binary black holes. We derive post-Newtonian accurate relations between different definitions of eccentricity. Based on these analyses, we introduce a new definition of eccentricity based on the (2,2)-mode of the gravitational radiation, which reduces to the Newtonian definition of eccentricity in the Newtonian limit. From the comparison between NR simulations and SMR results, we quantify the unknown next-to-leading order SMR contributions to the gravitational energy and angular momentum fluxes, and periastron advance. We show that in the comparable mass regime these contributions are subdominant and higher order SMR contributions are negligible.
AB - The modeling of unequal mass binary black hole systems is of high importance to detect and estimate parameters from these systems. Numerical relativity (NR) is well suited to study systems with comparable component masses, m1 similar to m2, whereas small mass ratio (SMR) perturbation theory applies to binaries where q = m2/m1 MUCH LESS-THAN 1. This work investigates the applicability for NR and SMR as a function of mass ratio for eccentric nonspinning binary black holes. We produce 52 NR simulations with mass ratios between 1:10 and 1:1 and initial eccentricities up to 0.8. From these we extract quantities like gravitational wave energy and angular momentum fluxes and periastron advance, and assess their accuracy. To facilitate comparison, we develop tools to map between NR and SMR inspiral evolutions of eccentric binary black holes. We derive post-Newtonian accurate relations between different definitions of eccentricity. Based on these analyses, we introduce a new definition of eccentricity based on the (2,2)-mode of the gravitational radiation, which reduces to the Newtonian definition of eccentricity in the Newtonian limit. From the comparison between NR simulations and SMR results, we quantify the unknown next-to-leading order SMR contributions to the gravitational energy and angular momentum fluxes, and periastron advance. We show that in the comparable mass regime these contributions are subdominant and higher order SMR contributions are negligible.
KW - POPULATION PROPERTIES
KW - CELESTIAL MECHANICS
KW - LIGO
KW - 1ST
U2 - 10.1103/PhysRevD.106.124040
DO - 10.1103/PhysRevD.106.124040
M3 - Journal article
VL - 106
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 12
M1 - 124040
ER -
ID: 337353082