Chern–Simons modified general relativity

Alexander, Stephon; Yunes, Nicolás

doi:10.1016/j.physrep.2009.07.002

Cited by 680 publications

(780 citation statements)

References 197 publications

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“…We investigated the nature of GW150914 by performing a series of tests devised to detect inconsistencies with the predictions of GR. With the exception of the graviton Compton wavelength and the test for the presence of a non-GR polarization, we did not perform any studies aimed at constraining parameters that might arise from specific alternative theories [13,14,88], such as Einstein-aether theory [105] and dynamical Chern-Simons theory [106], or from compact-object binaries composed of exotic objects such as boson stars [107] and gravastars [108]. Studies of this kind are not yet possible since we lack predictions for what the inspiral-merger-ringdown GW signal should look like in those cases.…”

Section: Prl 116 221101 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 99%

Tests of General Relativity with GW150914

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. Lett.

1,722

1,699

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The LIGO detection of GW150914 provides an unprecedented opportunity to study the two-body motion of a compact-object binary in the large-velocity, highly nonlinear regime, and to witness the final merger of the binary and the excitation of uniquely relativistic modes of the gravitational field. We carry out several investigations to determine whether GW150914 is consistent with a binary black-hole merger in general relativity. We find that the final remnant's mass and spin, as determined from the low-frequency (inspiral) and high-frequency (postinspiral) phases of the signal, are mutually consistent with the binary black-hole solution in general relativity. Furthermore, the data following the peak of GW150914 are consistent with the least-damped quasinormal mode inferred from the mass and spin of the remnant black hole. By using waveform models that allow for parametrized general-relativity violations during the inspiral and merger phases, we perform quantitative tests on the gravitational-wave phase in the dynamical regime and we determine the first empirical bounds on several high-order post-Newtonian coefficients. We constrain the graviton Compton wavelength, assuming that gravitons are dispersed in vacuum in the same way as particles with mass, obtaining a 90%-confidence lower bound of 10 13 km. In conclusion, within our statistical uncertainties, we find no evidence for violations of general relativity in the genuinely strong-field regime of gravity.

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Section: Prl 116 221101 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 99%

Tests of General Relativity with GW150914

Abbott¹,

Abbott²,

Abbott³

et al. 2016

Phys. Rev. Lett.

1,722

1,699

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show abstract

“…For example, without prior knowledge of the spin magnitudes and component masses, they find that Einsteindilaton Gauss-Bonnet [67], dynamical Chern-Simons [68,69,70], and scalar-tensor theories (e.g., [71]) cannot be constrained meaningfully because of degeneracies with the masses and spins, and Einstein-AEther theory [72,73] and ideas involving extra dimensions ( [74]; see [75] for a limit based on the lack of Hawking evaporation of black holes in globular clusters) or time variation of Newton's constant G [76] are better constrained by other measurements, particularly those of binary pulsars.…”

Section: Tests Of Gravity With Gw150914mentioning

confidence: 99%

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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“…2 A poloidal magnetic field structure that arises naturally from binary neutron-star coalescence, as computed using fully general-relativistic MHD [14]. look for birefringence in the propagation of gravitational waves, something again that is possible in modified theories of gravity [17].…”

Section: Neutron Star Binary Coalescencementioning

confidence: 99%