Derives first-order EM perturbation equations from covariant Maxwell equations in GW backgrounds, shows equivalence of formulations, and calculates that typical GW strains of 10^{-21} induce EM responses of order 10^{-19} relative to incident fields.
Signal Photon Flux and Background Noise in a Coupling Electromagnetic Detecting System for High Frequency Gravitational Waves
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abstract
A coupling system between Gaussian type-microwave photon flux, static magnetic field and fractal membranes (or other equivalent microwave lenses) can be used to detect high-frequency gravitational waves (HFGWs) in the microwave band. We study the signal photon flux, background photon flux and the requisite minimal accumulation time of the signal in the coupling system. Unlike pure inverse Gertsenshtein effect (G-effect) caused by the HFGWs in the GHz band, the the electromagnetic (EM) detecting scheme (EDS) proposed by China and the US HFGW groups is based on the composite effect of the synchro-resonance effect and the inverse G-effect. Key parameters in the scheme include first-order perturbative photon flux (PPF) and not the second-order PPF; the distinguishable signal is the transverse first-order PPF and not the longitudinal PPF; the photon flux focused by the fractal membranes or other equivalent microwave lenses is not only the transverse first-order PPF but the total transverse photon flux, and these photon fluxes have different signal-to-noise ratios at the different receiving surfaces. Theoretical analysis and numerical estimation show that the requisite minimal accumulation time of the signal at the special receiving surfaces and in the background noise fluctuation would be $\sim10^3-10^5$ seconds for the typical laboratory condition and parameters of $h_{r.m.s.}\sim10^{-26}-10^{-30}$ at 5GHz with bandwidth $\sim$1Hz. In addition, we review the inverse G-effect in the EM detection of the HFGWs, and it is shown that the EM detecting scheme based only on the pure inverse G-effect in the laboratory condition would not be useful to detect HFGWs in the microwave band.
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Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.
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First-Order Perturbations of Covariant Maxwell Equations in Gravitational Waves
Derives first-order EM perturbation equations from covariant Maxwell equations in GW backgrounds, shows equivalence of formulations, and calculates that typical GW strains of 10^{-21} induce EM responses of order 10^{-19} relative to incident fields.
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Self-resonance preheating in deformed attractor models: oscillon formation and evolution
Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency gravitational wave tail while leaving low frequencies unchanged.