Sourced Scalar Fluctuations in Bouncing Cosmology

Abstract

We calculate the scalar power spectrum generated by sourced fluctuations due to coupling between the scalar field, which holds most of the energy density of the universe, and a gauge field for a general FLRW metric. For this purpose we calculate the curvature perturbation to second order in the presence of gauge fields, and show that the gauge fields behave like an additional potential term. We then apply the analysis to the case of slow-contraction. Due to the interaction between the scalar field and gauge fields additional 'sourced' tensor and scalar spectra are generated. The resulting spectra are chiral, slightly blue and arbitrarily close to scale invariance. The only difference between the tensor and scalar spectra is the coupling constant with an $\mathcal{O}(1)$ numerical coefficient, and some momentum space polarization vectors. As a result the tilt of the spectra are the same. For the nearly scale invariant case, the momentum integration gives the same leading contribution. Hence, $r\simeq 1/9$ where the deviation from this value is controlled by the deviation from scale invariance, and is not in agreement with CMB observations. Deviating considerably from near scale invariance, and considering a bluer tilt with $n_T>0.12$, the model cannot account for CMB observations, but can be detected by LIGO and/or LISA in the future.

Corrected an error in writing the coupling to the gauge field in terms of the scalar field and the corresponding equations. As a result, the prediction is r=1/9. Matches the published erratum

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Cited by in corpus (7)

• Cosmology with the Laser Interferometer Space Antenna
• Probing The Early Universe Cosmology With NANOGrav: Possibilities and Limitations
• Islands in the Fluid: Islands are Common in Cosmology
• Gravitational-wave background in bouncing models from semi-classical, quantum and string gravity
• Sourced fluctuations in generic slow contraction
• Banks-Zaks Cosmology, Inflation, and the Big Bang Singularity
• The Grand Canonical Multiverse and the Small Cosmological Constant