Backreaction from inhomogeneous matter fields during large-scale structure formation

Abstract

We study how inhomogeneities of the cosmological fluid fields backreact on the homogeneous part of energy density and how they modify the Friedmann equations. In general, backreaction requires to go beyond the pressureless ideal fluid approximation, and this can lead to a reduced growth of cosmological large scale structure. Since observational evidence favours evolution close to the standard growing mode in the linear regime, we focus on two-component fluids in which the non-ideal fluid is gravitationally coupled to cold dark matter and in which a standard growing mode persists. This is realized, e.g. for a baryonic fluid coupled to cold dark matter. We calculate the backreaction for this case and for a wide range of other two-fluid models. Here the effect is either suppressed because the non-ideal matter properties are numerically too small, or because they lead to a too stringent UV cut-off of the integral over the power spectrum that determines backreaction. We discuss then matter field backreaction from a broader perspective and generalize the formalism such that also far-from-equilibrium scenarios relevant to late cosmological times and non-linear scales can be addressed in the future.

11 pages, 3 figures

References in corpus (8)

• Generation of Vorticity and Velocity Dispersion by Orbit Crossing
• Does Bulk Viscosity Create a Viable Unified Dark Matter Model?
• Bulk Viscous Cosmology
• A new framework for analyzing the effects of small scale inhomogeneities in cosmology
• Bulk Viscosity, Decaying Dark Matter, and the Cosmic Acceleration
• Accelerating cosmological expansion from shear and bulk viscosity
• Late Decaying Dark Matter, Bulk Viscosity and the Cosmic Acceleration
• Renormalization-group flow of the effective action of cosmological large-scale structures