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Detecting high-frequency gravitational waves with optically-levitated sensors

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arxiv 1207.5320 v2 pith:4DEBRYVN submitted 2012-07-23 gr-qc astro-ph.IMhep-phphysics.atom-phphysics.optics

Asimina Arvanitaki , Andrew A. Geraci This is my paper
classification gr-qcastro-ph.IMhep-phphysics.atom-phphysics.optics
keywords gravitationaldetectfrequencyrangewavewavesaboveannihilation
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We propose a tunable resonant sensor to detect gravitational waves in the frequency range of 50-300 kHz using optically trapped and cooled dielectric microspheres or micro-discs. The technique we describe can exceed the sensitivity of laser-based gravitational wave observatories in this frequency range, using an instrument of only a few percent of their size. Such a device extends the search volume for gravitational wave sources above 100 kHz by 1 to 3 orders of magnitude, and could detect monochromatic gravitational radiation from the annihilation of QCD axions in the cloud they form around stellar mass black holes within our galaxy due to the superradiance effect.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Gravitational Photon Polarization Twist to Probe the Early Universe and the Galactic Center

    hep-ph 2025-07 conditional novelty 6.0 of 10

    A long-baseline laser pulse whose polarization is twisted by gravitational waves could detect galactic-center pulsar and early-universe gravitational wave backgrounds.

  2. High-Frequency Gravitational Waves on BREAD

    hep-ph 2025-05 conditional novelty 6.0 of 10

    BREAD with single photon detectors could detect high-frequency gravitational waves at 0.05 to 200 THz, with projected strains as low as 1e-25 at 200 THz.

  3. Gravitational Wave Spectrum from the Production of Dark Matter via the freeze-in Mechanism

    hep-ph 2025-08 conditional novelty 4.0 of 10

    Graviton bremsstrahlung during freeze-in dark matter production yields a high-frequency gravitational wave background peaking near 5.35 x 10^10 Hz, with UV freeze-in amplitudes up to Omega_GW h^2 ~ 1e-17.

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