Loop Corrections in Non-Linear Cosmological Perturbation Theory

Details Loop Corrections in Non-Linear Cosmological Perturbation Theory Loop Corrections in Non-Linear Cosmological Perturbation Theory

1995-09-07

arxiv.org/abs/astro-ph/9509047v1

Astrophys.J.Suppl.105:37,1996

Astronomy and Astrophysics

Astrophysics

53 pages, uuencoded and gzipped postscript file, 20 figures, 25 tables, also available at http://fnas08.fnal.gov/cumu.uu

Scientific paper

10.1086/192306

Using a diagrammatic approach to Eulerian perturbation theory, we analytically calculate the variance and skewness of the density and velocity divergence induced by gravitational evolution from Gaussian initial conditions, including corrections *beyond* leading order. Except for the power spectrum, previous calculations in cosmological perturbation theory have been confined to leading order (tree level)-we extend these to include loop corrections. For scale-free initial power spectra, the one-loop variance \sigma^2 = \sigma^2_l + 1.82 \sigma^4_l and the skewness S_3 = 34/7 + 9.8 \sigma^2_l, where \sigma_l is the rms fluctuation of the linear density field. We also compute loop corrections to the variance, skewness, and kurtosis for several non-linear approximation schemes, where the calculation can be easily generalized to 1-point cumulants of higher order and arbitrary number of loops. We find that the Zel'dovich approximation gives the best approximation to the loop corrections of exact perturbation theory, followed by the Linear Potential approximation (LPA) and the Frozen Flow approximation (FFA), in qualitative agreement with the relative behavior of tree-level results. In LPA and FFA, loop corrections are infrared divergent for spectral indices n < 0; this is related to the breaking of Galilean invariance in these schemes.

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