Inflation宇宙における密度ゆらぎと角パワースペクトラム
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概要
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The tiny anisotropies of cosmic microwave background(CMB) originate from geometrical inhomogeneity in the early universe, and such inhomogeneity is considered as a candidate for the origin of structure. The geometrical perturbations, which are caused by the quantum fluctuation of scalar fields in the inflationary universe, are strictly treated and look into their evolution under the general relativity. In order to manage the freedom of gauge choice, we reconstruct the perturbed Einstein equations from the gauge-invariant quantities. The equation of motion for only metric perturbation is derived from the Einstein equations contained the matter and the geometrical quantity, and can be solved in the limited case. Here, in order to clarify a constraint from the matter to geometry, we calculate the second-order action of gravity and scalar field. Applying to the accelerated-expansion of the universe, we find that the evolution of metric perturbation will "freeze-in" in the midst of inflation, and that its spectrum is determined by potential of scalar field. We propose a scalar potential of inflation, motivated by modular invariant supergravity, and compute the angular power spectra of the adiabatic density perturbations that result from this model. The inflation predictions corresponding to this potential provide a good fit to the recent three-year WMAP data, e.g. the spectral index n_s=0.951. The TT and TE angular power spectra obtained from our model almost completely coincide with the corresponding results obtained from the ΛCDM model.
- 東海大学の論文
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