Nonsingular Model of the Universe with the Quantum-Gravitational de Sitter Stage and its Observational Consequences

Abstract

The standard Friedmann-Robertson-Walker cosmological model which is widely accepted now provides a good description of the modern state of our Universe, but it encounters a fundamental difficulty, namely, the existence of a singularity at some finite moment of time t = 0 in the past. The Friedman solution cannot be analytically continued to the region t < 0 where, strictly speaking, there is no space and no time. So, in the scope of classical general relativity, it is in principle impossible to ask what was the state of our Universe before t = 0. Thus a bound to the human cognition is set here. The consideration of more general inhomogeneous and anisotropic cosmological models does not improve the situation because, as is well known, these models are also singular.¹