Go to previous page Go up Go to next page

7 Structure Formation in the Early Universe

Structure formation in the early universe is a key problem in modern cosmology. It is believed that galaxies, clusters and all large-scale structures observed today originated from random sources of primordial inhomogeneities (density contrast) in the early universe, amplified by the expansion of the universe. Theories of structure formation based on general relativity theory have been in existence for over 60 years [27, 241, 242] (see, e.g., [17Jump To The Next Citation Point, 284Jump To The Next Citation Point, 300]), long before the advent of inflationary cosmology [233Jump To The Next Citation Point, 245Jump To The Next Citation Point, 269]. But the inflation paradigm [2, 140, 243, 244] provided at least two major improvements in the modern theory of cosmological structure formation [19, 141, 159, 270Jump To The Next Citation Point]:

Stochastic gravity provides a sound and natural formalism for the derivation of the cosmological perturbations generated during inflation. In [316Jump To The Next Citation Point] it was shown that the correlation functions that follow from the Einstein–Langevin equation, which emerges in the framework of stochastic gravity, coincide with that obtained with the usual quantization procedures [270Jump To The Next Citation Point] when both the metric perturbations and the inflaton fluctuations are linearized. Stochastic gravity, however, can naturally deal with the fluctuations of the inflaton field even beyond the linear approximation. In Section 7.4 we will enumerate possible advantages of the stochastic-gravity treatment of this problem over the usual methods based on the quantization of the linear cosmological and linear inflaton perturbations.

We should point out that the equivalence at the linearized level is proved in [316Jump To The Next Citation Point] directly from the field equations of the perturbations and by showing that the stochastic and the quantum correlations are both given by identical expressions. Within the stochastic gravity framework an explicit computation of the curvature perturbation correlations was performed by Urakawa and Maeda [353Jump To The Next Citation Point]. A convenient approximation for that computation, used by these authors, leads only to a small discrepancy with the usual approach for the observationally relevant part of the spectrum. We think the deviation from the standard result found for superhorizon modes would not arise if an exact calculation were used.

Here we illustrate the equivalence with the conventional approach with one of the simplest chaotic inflationary models in which the background spacetime is a quasi de Sitter universe [315Jump To The Next Citation Point, 316Jump To The Next Citation Point].

 7.1 The model
 7.2 Einstein–Langevin equation for scalar metric perturbations
 7.3 Correlation functions for scalar metric perturbations
 7.4 Summary and outlook

  Go to previous page Go up Go to next page