Structure Formation, Backreaction and Weak Gravitational Fields

Details Structure Formation, Backreaction and Weak Gravitational Fields Structure Formation, Backreaction and Weak Gravitational Fields

2008-01-10

arxiv.org/abs/0801.1546v3

JCAP 0803:023,2008

Astronomy and Astrophysics

Astrophysics

20 pages, 14 figures; v3 -- Added material, scale dependence of backreaction highlighted; 2 figures and 1 reference added; con

Scientific paper

10.1088/1475-7516/2008/03/023

There is an ongoing debate in the literature as to whether the effects of averaging out inhomogeneities (``backreaction'') in Cosmology can be large enough to account for the acceleration of the scale factor in the FLRW models. In particular, some simple models of structure formation studied in the literature seem to indicate that this is indeed possible, and it has also been suggested that the perturbed FLRW framework is no longer a good approximation during structure formation, when the density contrast becomes nonlinear. In this work we attempt to clarify the situation to some extent, using a fully relativistic model of pressureless spherical collapse. We find that whereas averaging during structure formation can lead to acceleration via a selective choice of averaging domains, the acceleration is not present when more generic domains are used for averaging. Further, we show that for most of the duration of the collapse, matter velocities remain small, and the perturbed FLRW form of the metric can be explicitly recovered, in the structure formation phase. We also discuss the fact that the magnitude of the average effects of inhomogeneities depends on the scale of averaging, and while it may not be completely negligible on intermediate scales, it is expected to remain small when averaging on suitably large scales.

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