Searcharxiv⌕ Search

arXiv · 2609.32905

Gravitational-Wave Modulation of Atomic Spontaneous Emission: Electrodynamical Theory, Quadrupolar Redistribution, and Rydberg Cavity Metrology

Abstract

Studying Gravitational Waves (GWs) provide a unique probe of the interplay between quantum matter and the dynamics of spacetime. We develop a QED framework for spontaneous emission in the presence of a weak classical GW by quantizing the electromagnetic field in a linearized gravitational background. We show that a passing GW dynamically phase-modulates vacuum electromagnetic modes, dressing photon states into a Floquet ladder of sidebands separated by the GW frequency. While the total spontaneous decay rate remains unchanged to first order in the GW strain, the emission pattern develops a characteristic spin-2 quadrupolar angular redistribution modulated with the GW phase. For finite interaction times, interference between the carrier and Floquet sidebands generates phase-dependent spectral asymmetries in the transient emission spectrum. To explore experimental observability, we formulate a cavity-QED master equation description and propose a differential cross-cavity detection protocol employing Rydberg ensembles or highly charged ions. These results establish cavity QED as a promising platform for exploring quantum electrodynamics in dynamical spacetime and for high-frequency gravitational-wave detection.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Sohrab Rahvar. 2026-09-26. Gravitational-Wave Modulation of Atomic Spontaneous Emission: Electrodynamical Theory, Quadrupolar Redistribution, and Rydberg Cavity Metrology. https://arxiv.org/abs/2609.32905

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

KEEP EXPLORING

Related papers

Quantum spacetime from constraints: wave equations and fields

In previous works, we showed that both time and space can emerge from entanglement within a globally constrained quantum Universe, with no background coordinates. By extending the Page and Wootters quantum time formalism to include both quantum clocks and rods, and imposing global constraints on total energy and momentum, we constructed a fully relational model of quantum spacetime. Here we take a further step: working in 1+1 dimensions, we show that the standard wave equations governing quantum particles (the Schrödinger, Klein-Gordon and Dirac equations) emerge naturally from this framework. The solutions of the equations are derived directly from the constraints, without assuming any external spacetime structure. The second quantization formalism is also implemented and discussed. Our results provide further support for the idea that quantum dynamics in spacetime may emerge from entanglement and constraints.

gr-qc↗

Cosmological Expansion with Global Phase Normalization by the Hubble Horizon

We argue that cosmological expansion is subject to a global phase normalization in the gravitational path integral, fixed by causal horizon boundary conditions rather than by local dynamics. In this formulation, the cosmological conformal factor is not a propagating degree of freedom but a global gauge variable fixed by the Hamiltonian constraint, rendering the conventional conformal-factor problem inapplicable. A de Sitter turning point $(q=-1)$ uniquely fixes the phase density $Λ= J$ as the leading order integrating factor when the horizon Clausius relation holds, where $J$ is the trace of the Schouten tensor of the cosmological background. We parameterize departures from equilibrium by a single variance parameter $β$ governing non-adiabatic background evolution over a Hubble time scale. The resulting Hubble expansion points to a phantom regime beyond $Λ$CDM without new degrees of freedom. It provides a natural origin for cosmological tensions expressed by cosmographic parameters, arising from global constraints that inhibit a stable de Sitter universe.

gr-qc↗

Cosmological implications for hairy black holes via spontaneous symmetry breaking: Are Hairy Black Holes Primordial?

We investigate whether hairy black holes generated through spontaneous symmetry breaking in Einstein-Scalar-Gauss-Bonnet (ESGB) theory, involving a complex scalar field with a global $U(1)$ symmetry, can be compatible with cosmological evolution. To this end, we introduce the ESGB theory with a scalar self-interaction that becomes relevant on cosmological scales while remaining negligible near the black hole. Owing to the time dependence of the GB term on cosmological scales, the scalar field dynamics in the evolving FLRW background differ qualitatively from those in the nearly static black hole background. In particular, for scalar-GB couplings compatible with hairy black hole formation, the effective potential supports a symmetry-broken vacuum throughout inflation. However, after inflation, a decelerated expansion changes the sign of the GB term, temporarily making the effective potential unbounded from below. As the GB contribution subsequently decreases, the scalar self-interaction eventually dominates and restores the symmetry. Within this schematic framework, we derive stringent constraints on the coupling strengths, the cutoff scale, and the black hole mass, which primarily arise for avoiding efficient tachyonic amplification of the scalar field perturbations during the unbounded phase. For cutoff scales compatible with both cosmological evolution and scalar hair formation, we find that only ultralight black holes with masses of the order of a few grams can develop scalar hair, identifying them as hairy primordial black holes.

gr-qc↗