Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · 0709.2373

The dark energy scale in superconductors: Innovative theoretical and experimental concepts

Christian Beck·Clovis Jacinto de Matos
View original source ↗Read source document ↗Export metadata ↓

Abstract

We revisit the cosmological constant problem using the viewpoint that the observed value of dark energy density in the universe actually represents a rather natural value arising as the geometric mean of two vacuum energy densities, one being extremely large and the other one being extremely small. The corresponding mean energy scale is the Planck-Einstein scale l_PE = (l_P l_E)^1/2 = (hbar G/ c^3 Lambda)^1/4 ~ 0.037 mm, a natural scale both for dark energy and the physics of superconductors. We deal with the statistics of quantum fluctuations underlying dark energy in superconductors and consider a scale transformation from the Planck scale to the Planck-Einstein scale which leaves the quantum physics invariant. Our approach unifies various experimentally confirmed or conjectured effects in superconductors into a common framework: Cutoff of vacuum fluctuation spectra, formation of Tao balls, anomalous gravitomagnetic fields, non-classical inertia, and time uncertainties in radioactive superconductors. We propose several new experiments which may further elucidate the role of the Planck-Einstein scale in superconductors.

Explore related subjects

gr-qc

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Christian Beck, Clovis Jacinto de Matos. 2008-04-24. The dark energy scale in superconductors: Innovative theoretical and experimental concepts. https://arxiv.org/abs/0709.2373

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

KEEP EXPLORING

Related papers

arXiv2026

A class of decelerating inhomogeneous cosmological models giving rise to accelerating FLRW universes at large scales

In this manuscript, we develop a class of inhomogeneous relativistic cosmological models with the following properties: (i) They contain cosmological observers to whom the spatial geometry and the expansion are homogeneous and isotropic; (ii) Matter behaves closely to dust, as it is formed by an ensemble of massive particles whose number density $4$-vector is conserved and reacts viscously to the local tidal forces; (iii) They generalize the dust FLRW model; (iv) They give rise to effective models on large scales that reproduce the FLRW behaviour with dust and a running dark-energy term, which appears as a backreaction effect from the local gravitational potential; (v) By suitably setting the distribution of energy in the current universe, the effective large-scale equation-of-state parameter can reproduce, in principle, any polynomial on the scale factor whose term of order zero is negative; (vi) The luminous distance observations imply an apparent large-scale acceleration, as the deceleration parameter is negative, while in reality the universe is decelerating.

gr-qc↗
arXiv2026

Radial Stability of Charged Interacting Quark Stars Revisited

An error in the charged quark star literature \cite{Goncalves:2020joq} has resulted in erroneous solutions to the radial stability equations for charged interacting quark stars in \cite{zhang:2021}. In this article we recalculate the fundamental radial eigenfrequencies for charged, interacting quark stars in general relativity and discuss any departure from previous results \cite{zhang:2021}. Most of the qualitative trends persist, but the magnitudes of the separation between the maximum mass and stability points on a given branch can change significantly. We also note that all branches in \cite{zhang:2021} that contained no stable solutions now have stable solutions in their corrected counterparts. The net effect is that in all of the studied cases charged quark stars have a greater range of stability than originally predicted. We also compare four recent observational constraints not included in previous studies, and find that these constraints are satisfied by a subset of the mass-radius relations we obtain.

gr-qc↗
arXiv2026

Grey-body factor from correspondence with quasinormal mode for gravitational perturbation of higher-dimensional Reissner-Nordström black hole

We study the correspondence between quasinormal modes (QNMs) and grey-body factors (GBFs) of higher-dimensional Reissner--Nordström black holes. Considering scalar, vector, and tensor gravitational perturbations, we systematically compute the QNMs and GBFs for each spacetime dimension and set of black-hole parameters to evaluate the analytical formula connecting them. QNMs are obtained by the continued fraction and the integration-through-midpoints methods depending on the singularity structure in the Frobenius series. We compare the GBFs determined by the correspondence using QNMs with those computed numerically. The correspondence performs well for scalar($+$), vector($+$), vector($-$), and tensor perturbations. For the scalar($-$) perturbation, the GBFs obtained by the correspondence deviate noticeably from the accurate GBFs for black holes with low to intermediate values of the charge in $D>6$. The correspondence recovers reasonable accuracy at higher charges, although the effective potential exhibits double peaks, contrary to the assumption underlying the Wentzel--Kramers--Brillouin (WKB)-based derivation of the correspondence. Whereas the accuracy decreases with increasing $D$ for other perturbation types, the correspondence for the scalar($-$) perturbation yields more accurate GBFs in $D=8$ than those in $D=7$. For near-extreme black holes, the correspondence offers a reliable approximation of GBFs for the vector($-$) perturbation, even though a double-peak potential occurs in $D>6$. These results suggest that the correspondence has a wider range of applicability than might be expected from the assumption of the WKB approach.

gr-qc↗