Sagnac delay in the Kerr-dS spacetime: Implications for Mach’s principle

Karimov, R. Kh.; Izmailov, R. N.; Garipova, G. M.; Nandi, K. K.

doi:10.1140/epjp/i2018-11919-x

Cited by 6 publications

(3 citation statements)

References 26 publications

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“…This observation has implications for the well known 'twin paradox', which is no paradox but a genuine prediction of special relativity. The synchrony gap between the flying clocks brought about by the inertial forces is exactly the age difference between the circumnavigating twins (neglecting velocity effects) [13][14][15]. The synchrony gap brought about by the inertial forces is exactly the age difference between the circumnavigating twins (neglecting velocity effects) [13].…”

Section: Global Navigation Satellite Systems (Gnss) Updatementioning

confidence: 99%

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Upper limit on NUT charge from the observed terrestrial Sagnac effect

Kulbakova

Karimov

Izmailov

et al. 2018

Class. Quantum Grav.

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The exact Sagnac delay in the Kerr-Taub-NUT (Newman-Unti-Tamburino) spacetime is derived in the equatorial plane for non-geodesic as well as geodesic circular orbits. The resulting formula, being exact, can be directly applied to motion in the vicinity of any spinning object including black holes but here we are considering only the terrestrial case since observational data are available. The formula reveals that, in the limit of spin a → 0, the delay does not vanish. This fact is similar to the non-vanishing of Lense-Thirring precession under a → 0 even though the two effects originate from different premises. Assuming a reasonable input that the Kerr-Taub-NUT corrections are subsumed in the average residual uncertainty in the measured Sagnac delay, we compute upper limits on the NUT charge n. It is found that the upper limits on n are far larger than the Earth's gravitational mass, which has not been detected in observations, implying that the Sagnac effect cannot constrain n to smaller values near zero. We find a curious difference between the delays for non-geodesic and geodesic clock orbits and point out its implication for the well known "twin paradox" of special relativity. * Electronic address: kulbakova.a@mail.ru † Electronic address: karimov ramis 92@mail.ru ‡ Electronic address: izmailov.

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Section: Global Navigation Satellite Systems (Gnss) Updatementioning

confidence: 99%

“…We shall point out that the difference in the delay for two types of orbits, non-geodesic and geodesic, in the flat space limit has an implication for twin paradox. Its implications for Mach's principle have been recently discussed elsewhere [14,15].…”

Section: Introductionmentioning

confidence: 97%

Upper limit on NUT charge from the observed terrestrial Sagnac effect

Kulbakova

Karimov

Izmailov

et al. 2018

Class. Quantum Grav.

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“…However, the delay in Eq. (16) is due to the physical effect of frame dragging [8] that gives rise also to a gravitational analogue of the Sagnac effect [20,21].…”

Section: Johannsen Metric and Relative Time Delaymentioning

confidence: 99%

Relative time delay in a spinning black hole as a diagnostic for no-hair theorem

Izmailov¹,

Zhdanov²,

Bhadra

et al. 2019

Eur. Phys. J. C

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The spinning regular black hole (spin a) metric proposed by Johannsen shares the Kerr horizon but contains independent dimensionless parameters marking deviation from the Kerr metric. Non-zero value of any of the parameters would indicate violation of the no-hair theorem. We shall find the influence of these parameters on the relative time delay (not Shapiro time delay) treated here as a diagnostic for no-hair theorem using aligned, finite, thinlens approximation in realistic spinning astrophysical configurations. Precise measurement of this delay would then help us determine, from observational perspective, whether or not any of the parameters is really non-zero. We shall also point out that the aligned spinning lens is completely equivalent to a "static" lens with a fictitious lens geometry, which would enable us to re-express the relative time delay components in terms of the spin a. Numerical values are tabulated for three astrophysical lens systems. The advantage of the present treatment is that it can accommodate a variety of spinning lens systems that are likely to be detected in the near future.

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