Perturbative photon fluxes generated by high-frequency gravitational waves and their physical effects

Abstract

We consider the electromagnetic (EM) perturbative effects produced by the high-frequency gravitational waves (HFGWs) in the GHz band in a special EM resonance system, which consists of fractal membranes, a Gaussian beam (GB) passing through a static magnetic field.It is predicted, under the synchroresonance condition, coherence modulation of the HFGWs to the preexisting transverse components of the GB produces the transverse perturbative photon flux (PPF),which has three novel and important properties: (1)The PPF has maximum at a longitudinal symmetrical surface of the GB where the transverse background photon flux (BPF) vanishes; (2) the resonant effect will be high sensitive to the propagating directions of the HFGWs; (3) the PPF reflected or transmitted by the fractal membrane exhibits a very small decay compared with very large decay of the much stronger BPF. Such properties might provide a new way to distinguish and display the perturbative effects produced by the HFGWs. We also discuss the high-frequency asymptotic behavior of the relic GWs in the microwave band and the positive definite issues of their energy-momentum pseudo-tensor .

Baryon asymmetry, dark matter, and density perturbation from primordial black holes

“…However, it is recently pointed out by refs. [65][66][67] that a new kind of detector has a capability of detecting high frequency gravitational waves by using the inverse Gertsenshtein effect [68]. In this section, we review the new detection scheme and discuss the possibility of testing our scenario.…”

“…Therefore, in refs. [65][66][67], a new technique is suggested. If one applies 0-th order electromagnetic waves ( E (0) , B (0) ) as a background, a first order signal flux n (1) appears as follows,…”

“…However, by use of optical ingenuities (e.g. a Gaussian beam and a Fractal membrane), one can distinguish n (1) from n (0) [65][66][67]. Thus the noise from n (0) is supposed to be negligible and the condition to detect the signal is estimated as n (1) ∆t > n th ∆t, (6.16) where ∆t is the detection time and n th is the flux of thermal noise.…”

“…(59) of ref. [66] the numerical values, 12 W 0 = 0.05m, l 1 = 0, x = 0.005m, y = 0.01m, z = 100m, ω e = 2πν g = 2π × 10 13 Hz, and multiplying A = 10 −4 m 2 , we obtain the signal flux as…”

Towards a New Era in Gravitational Wave Detection: High Frequency Gravitational Wave Research

“…Up to now, four groups worldwide are developing HFGW Detectors: one group at the Birmingham University, England, lead by Cruise (2000) another at the INFN Genoa, Italy, lead by Bernard (2002), the Chongqing University, China, lead by Li (2003); and the USA-based group GravWave, lead by Baker (2007). Recently, the last two have merged into a collaboration being the detector jointly developed referred as the Li-Baker detector (Li et al, 2008).…”