scholarly journals Binary black hole coalescence in the extreme-mass-ratio limit: Testing and improving the effective-one-body multipolar waveform

2011 ◽  
Vol 83 (6) ◽  
Author(s):  
Sebastiano Bernuzzi ◽  
Alessandro Nagar ◽  
Anıl Zenginoğlu
Keyword(s):  
Black Hole ◽  
Mass Ratio ◽  
Binary Black Hole ◽  
Ratio Limit

scholarly journals Binary black hole merger in the extreme-mass-ratio limit

2007 ◽  
Vol 24 (12) ◽  
pp. S109-S123 ◽  
Author(s):  
Alessandro Nagar ◽  
Thibault Damour ◽  
Angelo Tartaglia
Keyword(s):  
Black Hole ◽  
Mass Ratio ◽  
Binary Black Hole ◽  
Ratio Limit

scholarly journals Love in extrema ratio

2019 ◽  
Vol 28 (14) ◽  
pp. 1944001 ◽  
Author(s):  
Paolo Pani ◽  
Andrea Maselli
Keyword(s):  
Black Hole ◽  
Neutron Stars ◽  
Leading Order ◽  
Mass Ratio ◽  
Love Number ◽  
Space Antenna ◽  
Central Object ◽  
Love Numbers ◽  
Ratio Limit ◽  
Laser Interferometric

The tidal deformability of a self-gravitating object leaves an imprint on the gravitational-wave signal of an inspiral which is paramount to measure the internal structure of the binary components. We unveil here a surprisingly unnoticed effect: in the extreme mass-ratio limit the tidal Love number of the central object (i.e. the quadrupole moment induced by the tidal field of its companion) affects the gravitational waveform at the leading order in the mass ratio. This effect acts as a magnifying glass for the tidal deformability of supermassive objects but was so far neglected, probably because the tidal Love numbers of a black hole (the most natural candidate for a compact supermassive object) are identically zero. We argue that extreme mass-ratio inspirals detectable by the future laser interferometric space antenna (LISA) mission might place constraints on the tidal Love numbers of the central object which are roughly eight orders of magnitude more stringent than current ones on neutron stars, potentially probing all models of black hole mimickers proposed so far.

scholarly journals Who Ordered That? Unequal-mass Binary Black Hole Mergers Have Larger Effective Spins

2021 ◽  
Vol 922 (1) ◽  
pp. L5
Author(s):  
Thomas A. Callister ◽  
Carl-Johan Haster ◽  
Ken K. Y. Ng ◽  
Salvatore Vitale ◽  
Will M. Farr
Keyword(s):  
Black Hole ◽  
Odds Ratio ◽  
Hierarchical Analysis ◽  
Mass Ratio ◽  
Unequal Mass ◽  
Degree Correlation ◽  
Binary Black Hole ◽  
Formation And Evolution ◽  
The Mean

Abstract Hierarchical analysis of binary black hole (BBH) detections by the Advanced LIGO and Virgo detectors has offered an increasingly clear picture of their mass, spin, and redshift distributions. Fully understanding the formation and evolution of BBH mergers will require not just the characterization of these marginal distributions, but the discovery of any correlations that exist between the properties of BBHs. Here, we hierarchically analyze the ensemble of BBHs discovered by LIGO and Virgo with a model that allows for intrinsic correlations between their mass ratios q and effective inspiral spins χ eff. At 98.7% credibility, we find that the mean of the χ eff distribution varies as a function of q, such that more unequa-mass BBHs exhibit systematically larger χ eff. We find a Bayesian odds ratio of 10.5 in favor of a model that allows for such a correlation over one that does not. Finally, we use simulated signals to verify that our results are robust against degeneracies in the measurements of q and χ eff for individual events. While many proposed astrophysical formation channels predict some degree correlation between spins and mass ratio, these predicted correlations typically act in an opposite sense to the trend we observationally identify in the data.

scholarly journals Adapted gauge to small mass ratio binary black hole evolutions

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
Nicole Rosato ◽  
James Healy ◽  
Carlos O. Lousto
Keyword(s):  
Black Hole ◽  
Small Mass ◽  
Mass Ratio ◽  
Binary Black Hole

One parameter binary black hole inverse problem using a sparse training set

2018 ◽  
Vol 27 (04) ◽  
pp. 1850043 ◽  
Author(s):  
M. Carrillo ◽  
M. Gracia-Linares ◽  
J. A. González ◽  
F. S. Guzmán
Keyword(s):  
Black Hole ◽  
Time Domain ◽  
Signal To Noise Ratio ◽  
Small Sample ◽  
Mass Ratio ◽  
Training Set ◽  
The Core ◽  
Binary Black Hole ◽  
Orbital Phase ◽  
The Time Domain

In this paper, we use Artificial Neural Networks (ANNs) to estimate the mass ratio [Formula: see text] in a binary black hole collision out of the gravitational wave (GW) strain. We assume the strain is a time series (TS) that contains a part of the orbital phase and the ring-down of the final black hole. We apply the method to the strain itself in the time domain and also in the frequency domain. We present the accuracy in the prediction of the ANNs trained with various values of signal-to-noise ratio (SNR). The core of our results is that the estimate of the mass ratio is obtained with a small sample of training signals and resulting in predictions with errors of the order of 1% for our best ANN configurations.

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