Bounding the mass of the graviton using binary pulsar observations

Finn, L. S.; Sutton, P. J.

doi:10.1103/physrevd.65.044022

Cited by 170 publications

(209 citation statements)

References 19 publications

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“…Here ℓ P and M P are Planck length and mass respectively. Current observational bounds on the graviton mass from solar system measurements is m g < 4.4 × 10 −22 eV and its accuracy could be lowered up to m g < 10 −26 eV from future gravitational wave measurements [33,34,35,36]. Thus, our estimated theoretical value of the 'effective graviton mass' is well below the observational bound at present.…”

Section: Holonomy Correctionsmentioning

confidence: 69%

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Loop quantum gravity corrections to gravitational wave dispersion

2008

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Cosmological tensor perturbations equations are derived for Hamiltonian cosmology based on Ashtekar's formulation of general relativity, including typical quantum gravity effects in the Hamiltonian constraint as they are expected from loop quantum gravity. This translates to corrections of the dispersion relation for gravitational waves. The main application here is the preservation of causality which is shown to be realized due to the absence of anomalies in the effective constraint algebra used.

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Section: Holonomy Correctionsmentioning

confidence: 69%

“…This equation (35) describes propagating degrees of freedom which are the usual gravitational waves subject to quantum corrections. Unlike for inverse densitized triad corrections, the coefficients ofḧ i a and ∇ 2 h i a take the classical form.…”

Section: Linearized Equationmentioning

confidence: 99%

Loop quantum gravity corrections to gravitational wave dispersion

2008

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“…For example, if the dispersion measure of a massive graviton is assumed, GW150914 places an upper limit of mgc 2 < 2.2×10 −22 eV on the mass mg of the graviton ([64]; see [77] for the original proposal of this idea). This is significantly better than the limits available from Solar System [78] or binary pulsar [79] tests, and is also better than the limits that can be obtained by the lack of gravitational Cerenkov slowing of high-energy cosmic rays in certain parameter regimes [80]. There are slightly stronger, but more model-dependent, limits on the graviton mass that can be placed by the existence of stellar-mass black holes [81].…”

Section: Tests Of Gravity With Gw150914mentioning

confidence: 80%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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“…Ryan [15] has outlined how observations of the gravitational radiation from capture orbits of solar mass compact bodies about a supermassive black hole may allow the determination of certain multipole moments of the central hole, thereby testing the prediction of general relativity. More recently, Will [16] and Finn and Sutton [17,18] have described tests of general relativity that bound the mass of the graviton, and Scharre and Will [19] and Fairhurst et al [20] have shown how gravitational-wave observations of pulsars may be used to bound the value of the Brans-Dicke coupling constant.…”

Section: Introductionmentioning

confidence: 99%

“…One set of tests, including [13,15,17,19], is based on energy conservation arguments: the observed evolution of a system or of the radiation from a system is related to the energy loss expected owing to the radiation. A second class of tests [12,14,20] focuses on the observed polarization modes of the field.…”

Section: Introductionmentioning

confidence: 99%

Black-hole spectroscopy: testing general relativity through gravitational-wave observations

Dreyer

Kelly

Krishnan

et al. 2004

Class. Quantum Grav.

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350

308

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Assuming that general relativity is the correct theory of gravity in the strongfield limit, can gravitational-wave observations distinguish between black holes and other compact object sources? Alternatively, can gravitationalwave observations provide a test of one of the fundamental predictions of general relativity: the no-hair theorem? Here we describe a definitive test of the hypothesis that observations of damped, sinusoidal gravitational waves originate from a black hole or, alternatively, that nature respects the general relativistic no-hair theorem. For astrophysical black holes, which have a negligible charge-to-mass ratio, the black-hole quasi-normal mode spectrum is characterized entirely by the black-hole mass and angular momentum and is unique to black holes. In a different theory of gravity, or if the observed radiation arises from a different source (e.g., a neutron star, strange matter or boson star), the spectrum will be inconsistent with that predicted for general relativistic black holes. We give a statistical characterization of the consistency between the noisy observation and the theoretical predictions of general relativity and a demonstration, through simulation, of the effectiveness of the test for strong sources.

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Bounding the mass of the graviton using binary pulsar observations

Cited by 170 publications

References 19 publications

Loop quantum gravity corrections to gravitational wave dispersion

Loop quantum gravity corrections to gravitational wave dispersion

Implications of the gravitational wave event GW150914

Black-hole spectroscopy: testing general relativity through gravitational-wave observations

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