Tomographic analysis of the De Sitter model in quantum and classical cosmology

TL;DR

This paper employs a tomographic approach to analyze quantum and classical cosmological models, exploring initial conditions, quantum-to-classical transition, and the role of the cosmological constant in universe evolution.

Contribution

It extends the tomographic method to quantum cosmology and investigates the quantum-classical transition and the cosmological constant's decay as a key factor.

Findings

Quantum to classical transition may be driven by cosmological constant decay.

Tomographic analysis unifies quantum and classical descriptions of the universe.

Initial conditions influence the universe's evolution and transition mechanisms.

Abstract

The importance of the tomographic approach is that either in quantum mechanics as in classical mechanics the state of a physical system is expressed with the same family of functions, the tomograms. The extension of this procedure to quantum cosmology is straightforward. But instead of using the tomographic representation, we use tomograms to analyze the properties of the quantum and classical universes, starting from the wave functions in quantum cosmology and the phase space distribution in classical cosmology. In this paper we resume the properties of the tomographic approach introduced in previous papers. Then we study and discuss the properties of the initial conditions introduced by Hartle and Hawking and by Vilenkin and Linde and we study their classical transition. It results that a possible reason for the quantum to classical transition is the decay of the cosmological constant from the Planck scale to the present one. So that the Cosmological Constant Problem becomes a crucial topic in study of the evolution of the universe.