Abstract
The black hole could have a primordial origin if its mass is less than 1M_odot . The mergers of these black hole binaries generate stochastic gravitational-wave background (SGWB). We investigate the SGWB in high frequency band 10^{8}–10^{10},mathrm {Hz}. It can be detected by high frequency gravitational-wave detector. Energy density spectrum and amplitude of the SGWB are derived. The upper limit of the energy density spectrum is around 10^{-7}. Also, the upper limit of the amplitude ranges from 10^{-31.5} to 10^{-29.5}. The fluctuation of spacetime origin from gravitational wave could give a fluctuation of the background electromagnetic field in a high frequency gravitational-wave detector. The signal photon flux generated by the SGWB in the high frequency band 10^{8}–10^{10},mathrm {Hz} is derived, which ranges from 1 to 10^2,mathrm {s^{-1}}. The comparison between the signal photon flux generated by relic gravitational waves (RGWs) and the SGWB is also discussed in this paper. It is shown that the signal photon flux generated by the RGW, which is predicted by the canonical single-field slow-roll inflation models, is sufficiently lower than the one generated by the SGWB in the high frequency band 10^{8}–10^{10},mathrm {Hz}. Our results indicate that the SGWB in the high frequency band 10^{8}–10^{10},mathrm {Hz} is more likely to be detected by the high frequency gravitational-wave detector.
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