Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 1808.08804

Recovering the Principle of Relativity from the Cosmic Fabric Model of Space

T. G. Tenev·M. F. Horstemeyer
View original source ↗Read source document ↗Export metadata ↓

Abstract

We extend the descriptive power of the Cosmic Fabric model of space developed by Tenev and Horstemeyer (2018) to include moving observers by demonstrating that all reference frames are phenomenologically equivalent with one another and transform between each other via the Lorentz transformations. Our approach is similar to that of Lorentz (1892), which was used to explain the negative outcome of the Michelson-Morley æther detection experiment (Michelson and Morley 1887), except that we deduce the notions of length contraction and time dilation from the postulates of the Cosmic Fabric model. Our result is valid for the continuum length scale at which, by definition, the cosmic fabric can be described mathematically as a continuum. Herein, we also discuss the length-scale dependent nature of the Cosmic Fabric model as a possible way to relate gravitational and quantum theories.

Explore related subjects

gr-qc

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

T. G. Tenev, M. F. Horstemeyer. 2018-08-22. Recovering the Principle of Relativity from the Cosmic Fabric Model of Space. https://doi.org/10.1142/s2424942418500111

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

KEEP EXPLORING

Related papers

arXiv2026

Red noise and evolving signals: a complete frequentist approach to supermassive black hole binary searches with pulsar timing arrays

Searches for gravitational waves (GWs) from isolated supermassive black hole binaries (SMBHBs) in pulsar timing array (PTA) data require simultaneous estimation of signal and noise parameters, so the dimensionality of the fit scales with the number of observed pulsars. This computational difficulty is exacerbated when source evolution from GW emission is included, since retaining both Earth and pulsar terms introduces the unknown pulsar distances. Existing frequentist methods such as the $\mathcal{F}$-statistic are restricted to non-evolving sources. In addition, they often rely on a noise covariance estimated from the same data and then held fixed during the signal search, which can bias parameter estimates. We present a Generalized Likelihood Ratio Test and the associated $\mathcal{T}$-statistic that overcomes the aforementioned limitations. This formulation extends earlier work in which the dimensionality of the fitting problem was drastically reduced by semi-analytical maximization of the likelihood over the pulsar phase parameters, followed by efficient global optimization over the remaining parameters using Particle Swarm Optimization. Our simulations demonstrate that for an evolving SMBHB signal with chirp mass $\mathcal{M}=10^{9.2} M_\odot$ and signal-to-noise ratio $20$, this detection statistic achieves a $100\%$ detection probability at a false-alarm probability of $0.06$ in a 30-pulsar timing array, which is characterized by a $100 \mathrm{ns}$ root-mean-square white noise residual and pulsar-specific red noise. For the 30-pulsar timing array at signal-to-noise ratio $10$ and false-alarm probability $0.06$, $\mathcal{T}$ detects $99/100$ realizations, outperforming the $\mathcal{F}_p$ statistic evaluated with the $H_0$-fitted covariance, which detects $71/100$ realizations.

gr-qc↗
arXiv2026

Null Completeness and Directional Rigidity in Bianchi I Spacetimes

A smooth Bianchi I spacetime satisfying the null convergence condition in every null direction is static if it contains a single null geodesic complete to both the past and the future. We prove this result for a general spatial metric, allowing non-diagonal evolution and arbitrary signs of the principal expansion rates. The proof starts from affine Raychaudhuri evolution. On a complete generator of a regular twist-free congruence, nonnegativity of an independent or fixed-ratio sharp-cutoff lower limit forces the full optical tensor to vanish. Dilated square weights give an exact sum rule equal to minus the total optical-square integral, with no assumed endpoint limits for the expansion. In Bianchi I, this optical saturation fixes the metric on the kernel of the conserved spatial covector. We classify the resulting geometry: a non-static metric has at most two saturated unoriented lines, corresponding to four oriented rays; two lines force diagonalizability by a constant spatial transformation, and a third forces staticity. Periodic and finite-duration geometries attain the bound. For finite pulses with a common static exterior, we derive the negative affine curvature integrals, their weak-amplitude angular dependence, and a nonperturbative bound on the metric excursion from three directional integral budgets. Saturated modes of a massless minimally coupled test scalar propagate without Bogoliubov mixing across the pulse. We also state the field-equation and averaged-energy assumptions under which these geometric results imply matter or semiclassical rigidity.

gr-qc↗
arXiv2026

Matter-induced global regularity in non-polynomial quasi-topological gravity with Born-Infeld electrodynamics

We construct exact static, spherically symmetric charged solutions in four-dimensional non-polynomial quasi-topological gravity coupled to Born-Infeld electrodynamics. We focus on the model $h(p)=p/(1+\ell^{2}p)$, whose vacuum branch develops a curvature singularity at a finite radius. We show that Born-Infeld nonlinearities can remove this singularity within a finite region of parameter space, yielding globally regular geometries with an asymptotically flat exterior and a finite-curvature AdS-type core. The regular sector contains both horizonless configurations and RBHs, separated by a degenerate-horizon boundary. We further identify a continuous branch of regular black holes with a triple-degenerate inner horizon and a simple outer event horizon, satisfying $κ_-=0$ and $κ_+\neq0$. These results provide a converse example to cases in which introducing charge spoils the regularity of a black hole that is regular in vacuum. In the present model, Born-Infeld electrodynamics instead removes the finite-radius singularity of a gravitational branch that is singular in vacuum and supports globally regular charged geometries, including regular black holes with nontrivial inner-horizon structure.

gr-qc↗