We propose a novel experiment to search for axion dark matter which differentiates the phase velocities of the left and right-handed polarized photons. Our optical cavity measures the difference of the resonant frequencies between two circular-polarizations of the laser beam. The design of our cavity adopts double-pass configuration to realize a null experiment and give a high common mode rejection of environmental disturbances. We estimate the potential sensitivity to the axion-photon coupling constant gaγ for the axion mass m 10 −10 eV. In a low mass range m 10 −15 eV, we can achieve gaγ 3 × 10 −16 GeV −1 which is beyond the current bound by several orders of magnitude.
Axion dark matter differentiates the phase velocities of the circular-polarized photons. In this Letter, a scheme to measure the phase difference by using a linear optical cavity is proposed. If the scheme is applied to the Fabry-Pérot arm of Advanced LIGO-like (Cosmic-Explorer-like) gravitational wave detector, the potential sensitivity to the axion-photon coupling constant, gaγ, reaches gaγ 8 × 10 −13 GeV −1 (4 × 10 −14 GeV −1 ) at the axion mass m 3 × 10 −13 eV (2 × 10 −15 eV) and remains at around this sensitivity for 3 orders of magnitude in mass. Furthermore, its sensitivity has a sharp peak reaching gaγ 10 −14 GeV −1 (8×10 −17 GeV −1 ) at m = 1.563×10 −10 eV (1.563 × 10 −11 eV). This sensitivity can be achieved without loosing any sensitivity to gravitational waves.
We study inflation driven by a dilaton and an axion, both of which are coupled to a SU(2) gauge field.We find that the inflation driven by the dilaton occurs in the early stage of inflation during which the gauge field grows due to the gauge kinetic function. When the energy density of magnetic fields catches up with that of electric fields, chromo-natural inflation takes over in the late stage of inflation, which we call delayed chromo-natural inflation. Thus, the delayed chromo-natural inflation driven by the axion and the gauge field is induced by the dilaton. The interesting outcome of the model is generation of chiral primordial gravitational waves on small scales. Since the gauge field is inert in the early stage of inflation, it is viable in contrast to the conventinal chromo-natural inflation. We find the parameter region where chiral gravitational waves are generated in a frequency range higher than nHz, which are potentially detectable in future gravitational wave interferometers and pulsar timing arrays such as DECIGO, eLISA and SKA.
We consider the inflationary universe with a spectator scalar field coupled to a U (1) gauge field and calculate curvature perturbation and gravitational waves (GWs). We find that the sourced GWs can be larger than the one from vacuum fluctuation and they are statistically anisotropic as well as linearly polarized. The GW power spectrum acquires higher multipole moments as P h ∝ (1 − cos 2 θ + cos 4 θ − cos 6 θ) irrespective of the model parameters.
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