Bounding the mass of the graviton with gravitational waves: Effect of spin precessions in massive black hole binaries

Stavridis, Adamantios; Will, Clifford M.

doi:10.1103/physrevd.80.044002

Cited by 79 publications

(42 citation statements)

References 31 publications

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“…A full noise analysis using proposed noise curves for the advanced LIGO and for LISA weakens these crude bounds by factors between two and 10 [423, 433, 41, 42, 23, 377, 445]. For example, for the inspiral of two 10 6 M ⊙ black holes with aligned spins at a distance of 3 Gpc observed by LISA, a bound of 2 × 10 16 km could be placed [41].…”

Section: Gravitational-wave Tests Of Gravitational Theorymentioning

confidence: 99%

The Confrontation between General Relativity and Experiment

Will

2014

Living Rev. Relativ.

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2,618

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The status of experimental tests of general relativity and of theoretical frameworks for analyzing them is reviewed and updated. Einstein’s equivalence principle (EEP) is well supported by experiments such as the Eötvös experiment, tests of local Lorentz invariance and clock experiments. Ongoing tests of EEP and of the inverse square law are searching for new interactions arising from unification or quantum gravity. Tests of general relativity at the post-Newtonian level have reached high precision, including the light deflection, the Shapiro time delay, the perihelion advance of Mercury, the Nordtvedt effect in lunar motion, and frame-dragging. Gravitational wave damping has been detected in an amount that agrees with general relativity to better than half a percent using the Hulse-Taylor binary pulsar, and a growing family of other binary pulsar systems is yielding new tests, especially of strong-field effects. Current and future tests of relativity will center on strong gravity and gravitational waves.

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Section: Gravitational-wave Tests Of Gravitational Theorymentioning

confidence: 99%

The Confrontation between General Relativity and Experiment

Will

2014

Living Rev. Relativ.

Self Cite

2,618

2,346

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“…This predicted bound would be weakened by about an order of magnitude for massive black holes with aligned, non-precessing spins (Berti et al, 2005;Scharre and Will, 2002); however, in a generic case once the effect of spin precession is incorporated, the bound can be restored (Stavridis and Will, 2009). For very massive black hole binaries, the bound can be raised by an order of magnitude when the gravitational waveform templates are improved by higher harmonics (Arun and Will, 2009;Huwyler et al, 2012).…”

Section: Modified Dispersion Relationmentioning

confidence: 99%

Graviton mass bounds

et al. 2017

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Recently, aLIGO has announced the first direct detections of gravitational waves, a direct manifestation of the propagating degrees of freedom of gravity. The detected signals GW150914 and GW151226 have been used to examine the basic properties of these gravitational degrees of freedom, particularly setting an upper bound on their mass. It is timely to review what the mass of these gravitational degrees of freedom means from the theoretical point of view, particularly taking into account the recent developments in constructing consistent massive gravity theories. Apart from the GW150914 mass bound, a few other observational bounds have been established from the effects of the Yukawa potential, modified dispersion relation and fifth force that are all induced when the fundamental gravitational degrees of freedom are massive. We review these different mass bounds and examine how they stand in the wake of recent theoretical developments and how they compare to the bound from GW150914.

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“…Will obtained the additional contributions to the GW phasing formula in Brans-Dicke theories [14] and massive graviton theories [15] as a one-parameter deviation from GR and discussed the bounds possible on these corresponding parameters from GW observations. These ideas were elaborated on in greater detail in a series of papers [16][17][18][19][20][21], studying how various physical effects in the binary affect the bounds. It is worth noting that these bounds possible on massive graviton theories will be complementary to those which are obtained by binary pulsar observations (see e.g.…”

Section: A Gravitational Waves and Tests Of Grmentioning

confidence: 99%

Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope

Arun²,

et al. 2010

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General relativity has very specific predictions for the gravitational waveforms from inspiralling compact binaries obtained using the post-Newtonian (PN) approximation. We investigate the extent to which the measurement of the PN coefficients, possible with the second generation gravitational-wave detectors such as the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) and the third generation gravitational-wave detectors such as the Einstein Telescope (ET), could be used to test post-Newtonian theory and to put bounds on a subclass of parametrized-post-Einstein theories which differ from general relativity in a parametrized sense. We demonstrate this possibility by employing the best inspiralling waveform model for nonspinning compact binaries which is 3.5PN accurate in phase and 3PN in amplitude. Within the class of theories considered, Advanced LIGO can test the theory at 1.5PN and thus the leading tail term. Future observations of stellar mass black hole binaries by ET can test the consistency between the various PN coefficients in the gravitational-wave phasing over the mass range of 11-44M . The choice of the lower frequency cutoff is important for testing post-Newtonian theory using the ET. The bias in the test arising from the assumption of nonspinning binaries is indicated.

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Bounding the mass of the graviton with gravitational waves: Effect of spin precessions in massive black hole binaries

Cited by 79 publications

References 31 publications

The Confrontation between General Relativity and Experiment

The Confrontation between General Relativity and Experiment

Graviton mass bounds

Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope

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