The Polarizations of Gravitational Waves

Gong, Yungui; Hou, S.

doi:10.3390/universe4080085

Cited by 48 publications

(45 citation statements)

References 73 publications

(96 reference statements)

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“…GWs propagate with the speed of light transverse to the direction of propagation and they have only two tensor polarizations in the theory of general relativity. Due to the possible existence of extra fields, GWs in alternative theories beyond general relativity may have up to six polarizations [8][9][10][11][12][13][14][15], so the nature of gravity can be probed by the detection of the polarization content of GWs. To detect the polarization content of short duration GWs and probe the nature of gravity, more detectors are needed.…”

Section: Introductionmentioning

confidence: 99%

Frequency response of space-based interferometric gravitational-wave detectors

et al. 2019

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Gravitational waves are perturbations of the metric of space-time. Six polarizations are possible, although general relativity predicts that only two such polarizations, tensor plus and tensor cross are present for gravitational waves. We give the analytical formulas for the antenna response functions for the six polarizations which are valid for any equal-arm interferometric gravitationalwave detectors without optical cavities in the arms. The response function averaged over the source direction and polarization angle decreases at high frequencies which deteriorates the signal-to-noise ratio registered in the detector. At high frequencies, the averaged response functions for the tensor and breathing modes fall of as 1/f 2 , the averaged response function for the longitudinal mode falls off as 1/f and the averaged response function for the vector mode falls off as ln(f )/f 2 . *

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Section: Introductionmentioning

confidence: 99%

Frequency response of space-based interferometric gravitational-wave detectors

et al. 2019

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“…GWs have polarizations [48,49]. To express the polarizations in a convenient way, one associates the graviton with a tetrad basis {l µ , n µ , x µ , y µ }, which are parallel transported along the trajectory of the graviton, and satisfy −l µ n µ = x µ x µ = y µ y µ = 1 with the remaining contractions vanishing.…”

Section: The Propagation Of Gravitational Wavesmentioning

confidence: 99%

Gravitational lensing of gravitational waves: Rotation of polarization plane

2019

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Similar to the light, gravitational waves traveling in multiple paths may arrive at the same location if there is a gravitational lens on their way. Apart from the magnification of the amplitudes and the time delay between the gravitational wave rays, gravitational lensing also rotates their polarization planes and causes the gravitational wave Faraday rotation. The effect of the Faraday rotation is weak and can be ignored. The rotation of the polarization plane results in the changes in the antenna pattern function, which describes the response of the detector to its relative orientation to the gravitational wave. These effects are all reflected in the strain, the signal registered by the interferometers. The gravitational wave rays in various directions stimulate different strains, mainly due to different magnification factors, the phases and the rotation of the polarization plane. The phase difference mainly comes from the time delay. Moreover, the rotation of the polarization plane seemingly introduces the apparent vector polarizations, when these strains are compared with each other. Because of the smallness of the deflection angles, the effect of the rotation is also negligible. *

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“…The GW energy flux is then evaluable through a theory-dependent gravitational energy-momentum pseudotensor [55][56][57]. The relationships between other (massless) polarisation modes, if they exist in a theory, and the perturbed Weyl scalars are determined through the E(2) classification of the theory [50].…”

Section: B Perturbed Weyl Scalarsmentioning

confidence: 99%

Gravitational perturbations of a Kerr black hole inf(R)gravity

Suvorov

2019

Phys. Rev. D

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Modified theories of gravity are often built such that they contain general relativity as a limiting case. This inclusion property implies that the Kerr metric is common to many families of theories. For example, all analytic f (R) theories with vanishing constant term admit the Kerr solution. In any given theory, however, the response of the gravitational field to astrophysical disturbances is tied to the structure of the field equations. As such, even if black holes are Kerr, the underlying theory can, in principle, be probed through gravitational distortions. In this paper, we study linear perturbations of a Kerr black hole in f (R) gravity using the Newman-Penrose formalism. We show that, as in general relativity, the equations governing the perturbed metric, which depend on the quadratic term of the function f , completely decouple.

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The Polarizations of Gravitational Waves

Cited by 48 publications

References 73 publications

Frequency response of space-based interferometric gravitational-wave detectors

Frequency response of space-based interferometric gravitational-wave detectors

Gravitational lensing of gravitational waves: Rotation of polarization plane

Gravitational perturbations of a Kerr black hole inf(R)gravity

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