How does the photon’s spin affect gravitational wave measurements?

Marsot, Loïc

doi:10.1103/physrevd.100.064050

Cited by 2 publications

(2 citation statements)

References 61 publications

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“…A massless limit of these equations was derived by Souriau and Saturnini [28,29], and particular examples adapted to certain spacetimes have been discussed in Refs. [30][31][32]. Another commonly used method is the Wentzel-Kramers-Brillouin (WKB) approximation for various field equations on curved spacetimes.…”

Section: Introductionmentioning

confidence: 99%

Gravitational spin Hall effect of light

Joudioux

Dodin

et al. 2020

Phys. Rev. D

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The propagation of electromagnetic waves in vacuum is often described within the geometrical optics approximation, which predicts that wave rays follow null geodesics. However, this model is valid only in the limit of infinitely high frequencies. At large but finite frequencies, diffraction can still be negligible, but the ray dynamics becomes affected by the evolution of the wave polarization. Hence, rays can deviate from null geodesics, which is known as the gravitational spin Hall effect of light. In the literature, this effect has been calculated ad hoc for a number of special cases, but no general description has been proposed. Here, we present a covariant Wentzel-Kramers-Brillouin analysis from first principles for the propagation of light in arbitrary curved spacetimes. We obtain polarization-dependent ray equations describing the gravitational spin Hall effect of light. We also present numerical examples of polarization-dependent ray dynamics in the Schwarzschild spacetime, and the magnitude of the effect is briefly discussed. The analysis reported here is analogous to that of the spin Hall effect of light in inhomogeneous media, which has been experimentally verified.

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Section: Introductionmentioning

confidence: 99%

Gravitational spin Hall effect of light

Joudioux

Dodin

et al. 2020

Phys. Rev. D

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“…Using a multipole expansion of the energy-momentum tensor, the dynamics of massive spinning test particles has been extensively studied in the form of the Mathisson-Papapetrou-Dixon equations [47,53,68,15,16]. A massless limit of these equations was derived by Souriau and Saturnini [63,57], and particular examples adapted to certain spacetimes have been discussed in [25,24,46]. Another commonly used method is the Wentzel-Kramers-Brillouin (WKB) approximation for various field equations on curved spacetimes.…”

Section: Introductionmentioning

confidence: 99%

Gravitational spin Hall effect of light

Oancea,

Joudioux,

Dodin

et al. 2020

Preprint

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The propagation of electromagnetic waves in vacuum is often described within the geometrical optics approximation, which predicts that wave rays follow null geodesics. However, this model is valid only in the limit of infinitely high frequencies. At large but finite frequencies, diffraction can still be negligible, but the ray dynamics becomes affected by the evolution of the wave polarization. Hence, rays can deviate from null geodesics, which is known as the gravitational spin Hall effect of light. In the literature, this effect has been calculated ad hoc for a number for special cases, but no general description has been proposed. Here, we present a covariant WKB analysis from first principles for the propagation of light in arbitrary curved spacetimes. We obtain polarization-dependent ray equations describing the gravitational spin Hall effect of light. We also present numerical examples of polarization-dependent ray dynamics in the Schwarzschild spacetime, and the magnitude of the effect is briefly discussed. The analysis presented here is analogous to the spin Hall effect of light in inhomogeneous media, which has been experimentally verified.

show abstract

How does the photon’s spin affect gravitational wave measurements?

Cited by 2 publications

References 61 publications

Gravitational spin Hall effect of light

Gravitational spin Hall effect of light

Gravitational spin Hall effect of light

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