Density fluctuations in $κ$-deformed inflationary universe

Details Density fluctuations in $κ$-deformed inflationary universe Density fluctuations in $κ$-deformed inflationary universe

2005-06-27

arxiv.org/abs/gr-qc/0506122v3

Phys.Rev. D72 (2005) 103523

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

final revision; 19 pages, 3 figures; to appear in Phys. Rev. D

Scientific paper

10.1103/PhysRevD.72.103523

We study the spectrum of metric fluctuation in $\kappa$-deformed inflationary universe. We write the theory of scalar metric fluctuations in the $\kappa-$deformed Robertson-Walker space, which is represented as a non-local theory in the conventional Robertson-Walker space. One important consequence of the deformation is that the mode generation time is naturally determined by the structure of the $\kappa-$deformation. We expand the non-local action in $H^2/\kappa^2$, with $H$ being the Hubble parameter and $\kappa$ the deformation parameter, and then compute the power spectra of scalar metric fluctuations both for the cases of exponential and power law inflations up to the first order in $H^2/\kappa^2$. We show that the power spectra of the metric fluctuation have non-trivial corrections on the time dependence and on the momentum dependence compared to the commutative space results. Especially for the power law inflation case, the power spectrum for UV modes is weakly blue shifted early in the inflation and its strength decreases in time. The power spectrum of far-IR modes has cutoff proportional to $k^3$ which may explain the low CMB quadrupole moment.

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