Perturbative photon flux generated by high-frequency relic gravitational waves and utilization of them for their detection

TL;DR

This paper proposes a novel detection method for high-frequency relic gravitational waves using perturbative photon flux generated by their interaction with a Gaussian beam and fractal membranes, potentially enabling cosmological insights.

Contribution

It introduces a new detection scheme for high-frequency relic GWs utilizing perturbative photon flux and fractal membranes, with specific resonance conditions and measurable signals.

Findings

Estimated photon flux signals of ~400 to 1300 per second at 10^10Hz.

Detection of PPFs with signal-to-background ratios greater than one.

Potential to distinguish relic GWs from different cosmological models.

Abstract

There exist corresponding metric perturbations of the relic gravitational waves (GWs) in the region of approximately h~10^(-30)-10^(-32)in the GHz band. A detector for these GWs is described in which we measure the perturbative photon flux (PPF) or signal generated by such high-frequency relic GWs (HFRGWs) via a coupling system of fractal membranes and a Gaussian beam (GB) passing through a static magnetic field. It is found that under the synchro-resonance condition in which the frequency of the GB is set equal to the frequency of the expected HFRGWs (h~2.00*10^(-31), v_g=10^10Hz in the quintessential inflationary models (QIM) and h~6.32*10^(-31), v_g=10^10Hz in the pre-big bang scenario (PBBS) may produce the PPFs of ~4.04*10^2/s and ~1.27*10^3/s in a surface of 100cm^2 area at the waist of the GB, respectively. The relatively weak first-order PPF, directed at right angles to the expected HFRGWs, is reflected by fractal membrane and the resulting reflected PPF (signal) exhibits a very small decay in transit to the detector (tunable microwave receiver) compared with the much stronger background photon flux, which allows for detection of the reflected PPF with signal to background noise ratios greater than one at the distance of the detector. We also discuss the selection capability of system and directional sensitivity for the resonance components from the stochastic relic GW background. The resolution of tiny difference between the PPFs generated by the relic GWs in the QIM and in the PBBS may be established and will be of cosmological significance. PACS numbers: 04.30.Nk, 04.30.Db, and 98.80.Cq.