The Observation of Gravitational Waves from a Binary Black Hole Merger

By D. Reitze. 2016

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In Signal Processing

Citations in the corpus

Bounding the space of holographic CFTs with chaos (2016, background): “ degrees of freedom. In D>3 bulk dimensions, such processes do not require the introduction of matter: gravitons can create geometry, and destroy entanglement. In D= 3, unlike in higher dimensions [89], there are no gravitational waves: gravitons in AdS 3 live at the boundary, and the dynamics of”
Measuring the Binary Black Hole Mass Spectrum with an Astrophysically Motivated Parameterization (2018, methodology): “Accounting for these factors, we calculate Vobs(Θ), the sensitive volume for a binary with parameters Θ, following Abbott et al. (2016c), using semianalytic noise models corresponding to different sensitivities (Abbott et al. 2016e).”
INTEGRAL Detection of the First Prompt Gamma-Ray Signal Coincident with the Gravitational-wave Event GW170817 (2017, background): “The advent of advanced gravitational-wave (GW) detectors, which have been able to detect binary black hole mergers (Abbott et al. 2016a, 2016b, 2016c, 2017; LIGO Scientific Collaboration & Virgo Collaboration 2017a) and have the capability to detect a signal from nearby BNS mergers (Abbott et al.…”
Formation of Double Neutron Star Systems (2017, methodology): “After the recent success in detecting GW signals from merging BHs by advanced LIGO (Abbott et al. 2016b,a, 2017), it is also expected that GWs from merging DNS systems will be detected in the near future with LIGO and other detectors like VIRGO and KAGRA.”
Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “to experimental relativity (Sec.7.4) and to cosmology (Sec.7.5). 7.1. Nuclear Physics through Gravitational Wave Observations Recently, Adv. LIGO detected gravitational waves from black hole binaries [17,18], and it is likely that it will soon detect gravitational waves from neutron star binaries in”
Proposal for gravitational-wave detection beyond the standard quantum limit through EPR entanglement (2016, background): “Detection of gravitational waves from merging binary black holes (BBH) by the Laser Interferometer Gravitational-wave Observatory (LIGO) opened the era of gravitational wave astronomy [1].”
The global non-linear stability of the Kerr-de Sitter family of black holes (2016, methodology): “We have u=uN e +uTN e (1)+uTT , with  uN uTN uTT = C [1] ±  ũN ũTN ũTT  , C [1] ± =  q −1 0 0 ∓q−1 q 0 0 0 1  .”
Wormholes versus black holes: quasinormal ringing at early and late times (2016, background): “Owing to the recent detection of a gravitational wave signal, which may be radiation from a merger of two black holes [5, 6], there is the revival of interest in study of quasinormal modes of black holes.”
Assisted inspirals of stellar mass black holes embedded in AGN discs: solving the ‘final au problem’ (2016, background): “Advanced LIGO recently announced the discovery of the gravitational wave event GW150914, shown to be a BHB with initial component masses M1 ≈ 36M and M2 ≈ 29M (Abbott et al. 2016).”
Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions (2017, background): “…new era, the Laser Interferometer Gravitational-Wave Observatory (LIGO) has demonstrated the existence of binary stellar-mass black hole systems (Abbott et al. 2016a, 2016b, 2016c, 2017a, 2017b) and continues to monitor the sky with broadband detectors for gravitational waves from compact…”
Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, background): “The first four direct detections of gravitational waves (GWs, Abbott et al. 2016a,b,c, 2017; The LIGO Scientific Collaboration et al. 2017) revolutionised our knowledge of black hole binaries (BHBs).”