Search arXiv⌕ Search

arXiv · gr-qc/0208056

The One-Way Speed of Light on Rotating Earth and the Definition of the Meter

Abstract

Since 1983 the meter is defined to be the "length of the path travelled by light in vacuum during a time interval of 1/299792458 of a second". If there was exactly one single consistent method of synchronizing clocks, or if all corresponding methods were equivalent, one could infer from the validity of special relativity theory on a definite value of the one-way speed of light c in inertial frames. It is true that sufficiently slowly separated clocks always show middle in time reflection when sending and receiving light signals. But a simple consideration proves that the one-way speed of light is not a constant in rotating systems, in principle detectable with only one clock. On basis of a new internal synchronization method, this also affects all local inertial frames on rotating Earth, too, violating an absolute constancy of the one-way speed of light. This is not a contradiction to Einstein's original theory of relativity but to the present definition of the meter. Based on the constant local average value c of light going there and back, however, a modification for the definition of the meter is suggested, which would not depend on synchronization of any distant clocks. Appendix: FitzGerald-Lorentz contraction and time dilation, according to Einstein's generally accepted understanding, should be purely kinematic effects and would not need any dynamic explanation. But an analysis of Ehrenfest's paradox of the rotating disk shows that it is not possible to separate exactly relativistic kinematics from dynamics. The necessity of such a fundamental restriction is well known for a long time - though only from quantum mechanics till now.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Peter Ostermann. 2002-08-19. The One-Way Speed of Light on Rotating Earth and the Definition of the Meter. https://arxiv.org/abs/gr-qc/0208056

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

An upper bound on the minimum orbital period of black holes

Previous research has focused on establishing lower bounds on the minimum orbital period of black holes. In this work, we explore the complementary question of whether an upper bound exists for the minimum orbital period of black holes. We investigate the minimum orbital periods of three types of black holes: Schwarzschild, Reissner-Nordström and Kerr-Newman black holes. We find that the minimum orbital period of these black holes is bounded by an upper limit $T_{min} \leqslant 6\sqrt{3}πM$, where $M$ is the black hole mass. Our results suggest that this upper bound on the minimum orbital period may be a general property in black hole spacetimes.

gr-qc↗

Bounds on the minimum orbital period in the background of 5-dimensional charged black holes

In this paper, we study the upper and lower bounds on the minimum orbital period of 5-dimensional charged black holes. Our results indicate that the upper bound of the minimum orbital period corresponds to non-charged black holes, while the lower bound is achieved in the case of maximally charged black holes. We further establish precise analytical expressions for the upper and lower bounds of the minimum orbital period. Our findings provide valuable insights into 5-dimensional charged black holes and help constrain theoretical gravity models.

gr-qc↗

Analysis of minimum orbital periods around d-dimensional charged black holes

This paper investigates the bounds on the minimum orbital period for test objects around d-dimensional charged black holes in asymptotically flat spacetimes. We derive the exact critical radius and the minimum orbital period. We then prove analytically that the minimum orbital period decreases strictly as the charge of the black hole increases. Thus, the upper limit is reached for an uncharged black hole, while the lower limit is attained for a maximally charged one, and the two bounds take the closed form $\frac{2π(d-2)}{d-3}[(d-2)M]^{\frac{1}{d-3}}\leqslant T_{min} \leqslant 2π\sqrt{\frac{d-1}{d-3}}\,[(d-1)M]^{\frac{1}{d-3}}$. Since the minimum period equals $2π$ times the shadow radius, the upper bound is equivalently a universal upper bound on the shadow radius. These results improve our understanding of dynamics around d-dimensional black holes and impose constraints on candidate gravity theories.

gr-qc↗