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Probing the non-linear structure of general relativity with black hole binaries
General Relativity and Quantum Cosmology · Submitted 16 Apr 2006
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim LISA (EGO) will observe BBH inspirals with a signal-to-noise ratio of more than 1000 (100) and thereby test the self-consistency of each of the nine post-Newtonian coefficients that have so-far been computed, by measuring the lower order coefficients to a relative accuracy of $\sim 10^{-5}$ (respectively, $\sim 10^{-4}$) and the higher order coefficients to a relative accuracy in the range $10^{-4}$-0.1 (respectively, $10^{-3}$-1).
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The abstract, sentence by sentence
Observations of the inspiral of massive binary black holes (BBH) in the Laser Interferometer Space Antenna (LISA) and stellar mass binary black holes in the European Gravitational-Wave Observatory (EGO) offer an unique opportunity to test the non-linear structure of general relativity. For a binary composed of two non-spinning black holes, the non-linear general relativistic effects depend only on the masses of the constituents. In a recent letter, we explored the possibility of a test to determine all the post-Newtonian coefficients in the gravitational wave-phasing. However, mutual covariances dilute the effectiveness of such a test. In this paper, we propose a more powerful test in which the various post-Newtonian coefficients in the gravitational wave phasing are systematically measured by treating three of them as independent parameters and demanding their mutual consistency. LISA (EGO) will observe BBH inspirals with a signal-to-noise ratio of more than 1000 (100) and thereby test the self-consistency of each of the nine post-Newtonian coefficients that have so-far been computed, by measuring the lower order coefficients to a relative accuracy of $\sim 10^{-5}$ (respectively, $\sim 10^{-4}$) and the higher order coefficients to a relative accuracy in the range $10^{-4}$-0.1 (respectively, $10^{-3}$-1).
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Observations of the inspiral of massive binary black holes (BBH) in the Laser Interferometer Space Antenna (LISA) and stellar mass binary black holes in the European Gravitational-Wave Observatory (EGO) offer an unique opportunity to test the non-linear structure of general relativity. | background 1.00 | 0.07 | 0.06 | asserted 0.83 |
| s1 | For a binary composed of two non-spinning black holes, the non-linear general relativistic effects depend only on the masses of the constituents. | background 1.00 | 0.10 | 0.04 | asserted 1.00 |
| s2 | In a recent letter, we explored the possibility of a test to determine all the post-Newtonian coefficients in the gravitational wave-phasing. | background 0.86 | 0.83 | 0.03 | asserted 0.69 |
| s3 | However, mutual covariances dilute the effectiveness of such a test. | limitation 0.52 | 0.25 | 0.03 | asserted 1.00 |
| s4 | In this paper, we propose a more powerful test in which the various post-Newtonian coefficients in the gravitational wave phasing are systematically measured by treating three of them as independent parameters and demanding their mutual consistency. | contribution 0.73 | 0.75 | 0.56 | asserted 0.95 |
| s5 | LISA (EGO) will observe BBH inspirals with a signal-to-noise ratio of more than 1000 (100) and thereby test the self-consistency of each of the nine post-Newtonian coefficients that have so-far been computed, by measuring the lower order coefficients to a relative accuracy of $\sim 10^{-5}$ (respectively, $\sim 10^{-4}$) and the higher order coefficients to a relative accuracy in the range $10^{-4}$-0.1 (respectively, $10^{-3}$-1). | result 0.68 | 0.36 | 0.57 | asserted 0.95 |
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Original abstract
Observations of the inspiral of massive binary black holes (BBH) in the Laser Interferometer Space Antenna (LISA) and stellar mass binary black holes in the European Gravitational-Wave Observatory (EGO) offer an unique opportunity to test the non-linear structure of general relativity. For a binary composed of two non-spinning black holes, the non-linear general relativistic effects depend only on the masses of the constituents. In a recent letter, we explored the possibility of a test to determine all the post-Newtonian coefficients in the gravitational wave-phasing. However, mutual covariances dilute the effectiveness of such a test. In this paper, we propose a more powerful test in which the various post-Newtonian coefficients in the gravitational wave phasing are systematically measured by treating three of them as independent parameters and demanding their mutual consistency. LISA (EGO) will observe BBH inspirals with a signal-to-noise ratio of more than 1000 (100) and thereby test the self-consistency of each of the nine post-Newtonian coefficients that have so-far been computed, by measuring the lower order coefficients to a relative accuracy of $\sim 10^{-5}$ (respectively, $\sim 10^{-4}$) and the higher order coefficients to a relative accuracy in the range $10^{-4}$-0.1 (respectively, $10^{-3}$-1).
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References
How the literature uses it
55 arXiv papers cite this in 76 sentences
Papers citing it · 45 sentences without a confident label
Builds on it 1 paper
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The first method is an extension of the standard null parametrized test of GR for quasicircular binaries [ref] .
Parametrized tests of general relativity using eccentric compact binaries · Summary and conclusions · 0.97
Uses its method or tool 2 papers
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In these works they used the proposal of Ref. [ref] (described earlier) to test the PN coefficients of GR recasting it using Bayesian model selection.
Tests of General Relativity and Alternative theories of gravity using Gravitational Wave observations · Bayesian Inference and Tests of Gravity · 0.89
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For instance, here we deploy the parameterized tests of post-Newtonian (PN) coefficients which are designed to be sensitive to physical effects manifesting at different PN orders [ref] , and analytical phenomenological coefficients to model the intermediate and merger-ringdown regimes [ref] .
Unveiling Microlensing Biases in Testing General Relativity with Gravitational Waves · Introduction · 0.92
Cites it as background 27 papers
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* A model-agnostic residuals test, which subtracts out the best-matched GR-modeled CBC waveform from the data containing the GW signal, and checks if the statistical properties of the residual are consistent with noise [ref] * A test that probes the inspiral evolution of the CBC by searching for deviations in Post-Newtonian (PN) parameters of the GW signal [ref] * An inspiral-merger-ringdown consistency test (IMRCT) that compares and assesses the consistency between the low and high-frequency portions of the CBC signals [ref] * Propagation tests of GWs that compare their speed with respect to the speed of light [ref] as well as any modulations in the waveform due to finite-graviton-mass-driven velocity dispersion [ref] .
A study of the Inspiral-Merger-Ringdown Consistency Test with gravitational-wave signals from compact binaries in eccentric orbits · Introduction · 0.94
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In parametrized tests with circular binaries [ref] , the GR waveform is modified by adding phenomenological deviation parameters at each PN order that capture potential deviations from GR: $φ_i φ_i (1 + δφ̂_i)$.
Parametrized tests of general relativity using eccentric compact binaries · Parametrized tests of GR for circular binaries · 0.90
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In the second class of tests, GR is tested for self-consistency by treating some of the coefficients in the post-Newtonian (PN) expansion of the phasing as free variables rather than deterministic functions of the source parameters, and verifying whether the recovered values are consistent with GR predictions [ref] .
Testing general relativity with gravitational waves: a reality check · Introduction and main results · 0.87
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