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Primordial perturbations and inflation in holographic cosmology
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abstract
We consider an inflationary scenario in the holographic braneworld with a cosmological fluid occupying the 3+1 dimensional brane located at the holographic boundary of an asymptotic ADS$_5$ bulk. The contribution of the boundary conformal field can be represented as a modification of Einstein's equations on the boundary. Using these effective Einstein equations we calculate the cosmological perturbations and derive the corresponding power spectra assuming a general $k$-essence type of inflaton. We find that the braneworld scenario affects the scalar power spectrum only in the speed of sound dependence on the slow-roll parameters whereas there is no change in the tensor power spectrum. This implies that the changes in the spectral indices appear at the second order in the slow-roll parameter expansion.
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A scaling invariance of the perturbations in $k$-inflation models
A scaling invariance of k-inflation background equations allows parameter redefinitions that normalize the curvature perturbation spectrum at the CMB pivot scale without altering its shape.
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