paper

Macroscopic theory of dark sector

arXiv:1311.6694 · doi:10.1155/2014/586958

Abstract

A simple Lagrangian with squared covariant divergence of a vector field as a kinetic term turned out an adequate tool for macroscopic description of the dark sector. The zero-mass field acts as the dark energy. Its energy-momentum tensor is a simple additive to the cosmological constant. Massive fields ϕ_{I} with ϕ^{K}ϕ_{K}<0 and ϕ^{K}ϕ_{K}>0 describe two different forms of dark matter. The space-like (ϕ^{K}ϕ_{K}<0) massive vector field is attractive. It is responsible for the observed plateau in galaxy rotation curves. The time-like (ϕ^{K}ϕ_{K}>0) massive field displays repulsive elasticity. In balance with dark energy and ordinary matter it provides a four parametric diversity of regular solutions of the Einstein equations describing different possible cosmological and oscillating non-singular scenarios of evolution of the universe. In particular, the singular big bang turns into a regular inflation-like transition from contraction to expansion with the accelerate expansion at late times. The fine-tuned Friedman-Robertson-Walker singular solution is a particular limiting case at the boundary of existence of regular oscillating solutions in the absence of vector fields. The simplicity of the general covariant expression for the energy-momentum tensor allows to display the main properties of the dark sector analytically and avoid unnecessary model assumptions.

54 pages, 12 figures. Review article. See details in my original papers arXiv:1201.2562, arXiv:1303.7062

References in corpus (8)