A potential third-generation gravitational-wave detector based on autocorrelative weak-value amplification

Jing-Hui Huang; Fei-Fan He; Xue-Ying Duan; Guang-Jun Wang; Xiang-Yun Hu

doi:10.1088/1361-6382/aceb47

paper

A potential third-generation gravitational-wave detector based on autocorrelative weak-value amplification

arXiv:2306.06827 · doi:10.1088/1361-6382/aceb47

Abstract

Reducing noises and enhancing signal-to-noise ratios (SNRs) have become critical for designing third-generation gravitational-wave (GW) detectors with a GW strain of less than $1 0^{- 23}$ / $Hz$ . In this paper, we propose a potential third-generation GW detector based on autocorrelative weak-value amplification (AWVA) for GW detection with a strain of $h_{g} =$ $4 \times 1 0^{- 25}$ / $Hz$ . In our scheme, a GW event induces a phase difference $Δ ϕ$ by passing through an 11-bounce delay line, 10-km arm-length, zero-area Sagnac interferometer illuminated with a 1064-nm laser. Subsequently, $Δ ϕ$ is amplified as the parameter of post-selection by choosing the appropriate pre-selected state and coupling strength in AWVA. In particular, we theoretically investigate the AWVA measurements for GW detection within the frequency band of 200 Hz $\leq$ $f_{g}$ $\leq$ 800 Hz, considering Gaussian noises with negative-decibel SNRs. The peak response of the AWVA sensitivity $κ (f_{g})$ occurs at frequency $f_{g, ma x}$ = 500 Hz, which falls within the frequency band of interest of the current third-generation GW detectors. Our simulation results indicate that AWVA can demonstrate a measurable sensitivity of $Θ (f_{g})$ within the frequency band of interest. Moreover, the robustness of WVA shows promising potential in mitigating the effects of Gaussian noises.

arXiv comment21 pages, 6 figures

A potential third-generation gravitational-wave detector based on autocorrelative weak-value amplification

Abstract

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