scholarly journals Validating the effective-one-body numerical-relativity waveform models for spin-aligned binary black holes along eccentric orbits

2020 ◽  
Vol 101 (4) ◽  
Author(s):  
Xiaolin Liu ◽  
Zhoujian Cao ◽  
Lijing Shao
Keyword(s):  
Black Holes ◽  
Numerical Relativity ◽  
Binary Black Holes ◽  
Eccentric Orbits

scholarly journals Up-down instability of binary black holes in numerical relativity

2021 ◽  
Vol 103 (6) ◽  
Author(s):  
Vijay Varma ◽  
Matthew Mould ◽  
Davide Gerosa ◽  
Mark A. Scheel ◽  
Lawrence E. Kidder ◽  
...  
Keyword(s):  
Black Holes ◽  
Numerical Relativity ◽  
Binary Black Holes

scholarly journals The Evolutionary Evidence for Be/Black Hole Binaries

2000 ◽  
Vol 175 ◽  
pp. 689-692
Author(s):  
Natalya V. Raguzova ◽  
Vladimir M. Lipunov
Keyword(s):  
Black Holes ◽  
Binary Systems ◽  
Be Stars ◽  
Evolutionary Track ◽  
Binary Black Holes ◽  
Black Hole Binaries ◽  
Eccentric Orbits ◽  
Evolutionary Scenario ◽  
The Galaxy ◽  
Near Future

AbstractUsing a Monte Carlo simulation of the modern scenario of the evolution of binary systems (the “Scenario Machine”), we calculate the number of binary black holes with Be stars and their expected observational properties. So far, only two possible candidates for Be/BH binaries have been proposed among the observable sources, the superluminal source GRS 1915+105 in the Galaxy and RX J0117.6–7330 in the SMC. We obtained an evolutionary track that can lead to the formation of such systems. The modern evolutionary scenario predicts the existence of binary black holes on eccentric orbits around Be stars and such systems may be discovered in the near future.

scholarly journals Binary black holes, gravitational waves, and numerical relativity

2007 ◽  
Vol 78 ◽  
pp. 012010 ◽  
Author(s):  
Joan M Centrella ◽  
John G Baker ◽  
William D Boggs ◽  
Bernard J Kelly ◽  
Sean T McWilliams ◽  
...  
Keyword(s):  
Black Holes ◽  
Gravitational Waves ◽  
Numerical Relativity ◽  
Binary Black Holes

GRAVITATIONAL WAVEFORMS FOR BINARY BLACK HOLES

2011 ◽  
Vol 20 (10) ◽  
pp. 2081-2086
Author(s):  
BALA R IYER
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Numerical Relativity ◽  
Current Status ◽  
Next Generation ◽  
Binary Black Holes ◽  
Gravitational Wave Detectors ◽  
Body Method

Over the last decade gravitational waveforms of binary black holes have been investigated using a variety of approaches like the Multipolar post-Minkowskian formalism, Numerical Relativity and the Effective-One-Body method. We review these complementary approaches and summarize the current status of these investigations of relevance to construct the best templates for the next generation Advanced gravitational wave detectors.

scholarly journals A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical-relativity formalism

2021 ◽  
Author(s):  
Xiaolin Liu ◽  
Zhoujian Cao ◽  
Zong-Hong Zhu
Keyword(s):  
Black Holes ◽  
Inclination Angle ◽  
Source Localization ◽  
Numerical Relativity ◽  
Large Mass ◽  
Reference Frequency ◽  
Binary Black Holes ◽  
Higher Modes ◽  
Minimal Matching ◽  
Initial Orbit

Abstract We have previously constructed a waveform model, SEOBNRE, for spinning binary black hole moving along eccentric orbit based on effective-one-body (EOB) formalism. In the current paper, we update SEOBNRE waveform model in the following three respects. Firstly, we update the EOB dynamics from SEOBNRv1 to SEOBNRv4. Secondly we properly treat the Schott term which has been ignored in previous SEOBNRE. Thirdly, we construct a new factorized waveform including (l,|m|)=(2,2),(2,1),(3,3),(4,4) modes based on effective-one-body (EOB) formalism, which is valid for spinning binary black holes (BBH) in general equatorial orbit. Following our previous SEOBNRE waveform model, we call our new waveform model SEOBNREHM. The (l,|m|)=(2,2) mode waveform of SEOBNREHM can fit the original SEOBNRv4 waveform very well in the case of a quasi-circular orbit. We have validated SEOBNREHM waveform model through comparing the waveform against the Simulating eXtreme Spacetimes (SXS) catalog. The comparison is done for BBH with total mass in (20,200)M_sun using Advanced LIGO designed sensitivity. For the quasi-circular cases we have compared our (2,2) mode waveforms to the 281 numerical relativity (NR) simulations of BBH along quasi-circular orbits. All of the matching factors are bigger than 98\%. For the elliptical cases, 24 numerical relativity simulations of BBH along an elliptic orbit are used. For each elliptical BBH system, we compare our modeled gravitational polarizations against the NR results for different combinations of the inclination angle, the initial orbit phase and the source localization in the sky. We use the minimal matching factor respect to the inclination angle, the initial orbit phase and the source localization to quantify the performance of the higher modes waveform. We found that after introducing the higher modes, the minimum of the minimal matching factor among the 24 tested elliptical BBHs increases from 90\% to 98\%. Our SEOBNREHM waveform model can match all tested 305 SXS waveforms better than 98\% including highly spinning ($\chi=0.99$) BBH, highly eccentric ($e\approx0.6$ at reference frequency $Mf_0=0.002$) BBH and large mass ratio ($q=10$) BBH.

scholarly journals Comparison of post-Newtonian mode amplitudes with numerical relativity simulations of binary black holes

2020 ◽  
Vol 37 (6) ◽  
pp. 065006 ◽  
Author(s):  
S Borhanian ◽  
K G Arun ◽  
H P Pfeiffer ◽  
B S Sathyaprakash
Keyword(s):  
Black Holes ◽  
Numerical Relativity ◽  
Binary Black Holes
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