cosmological perturbation theory oor Spaans
cosmological perturbation theory
en
(astronomy) A mathematical theory that attempts to describe the evolution of the constituents of the universe following the Big Bang
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teoría perturbacional cosmológica
en
theory by which the evolution of structure is understood in the big bang model
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Cosmological perturbation theory, which describes the evolution of slight inhomogeneities in the early universe, has allowed cosmologists to precisely calculate the angular power spectrum of the radiation, and it has been measured by the recent satellite experiments (COBE and WMAP) and many ground and balloon-based experiments (such as Degree Angular Scale Interferometer, Cosmic Background Imager, and Boomerang).
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Before this epoch, the evolution of the universe could be understood through linear cosmological perturbation theory: that is, all structures could be understood as small deviations from a perfect homogeneous universe.
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Palabras llave: General relativity; perturbation theory; cosmology.
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Web and PhD course 'Theory of cosmological perturbations with applications to inflation and the late-time universe', 27 March to 5 April, at the Faculty of Physics.
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In the present work, we find, the field equations, the Friedmann equations for a homogeneous and isotropic universe and the cosmological perturbations for each of the theories previously exposed.
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In addition to finding the cosmological perturbations in a general way, these are calculated for a domain of matter domain, thus finding the Poisson equations for the Scalar-Tensor and f(R) gravity theories.
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