Equilibrium boundary conditions, dynamic vacuum energy, and the Big Bang

Details Equilibrium boundary conditions, dynamic vacuum energy, and the Big Bang Equilibrium boundary conditions, dynamic vacuum energy, and the Big Bang

2008-03-03

arxiv.org/abs/0803.0281v7

Phys.Rev.D78:083533,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

20 pages with revtex4; v7: published version in preprint style

Scientific paper

10.1103/PhysRevD.78.083533

The near-zero value of the cosmological constant \Lambda in an equilibrium context may be due to the existence of a self-tuning relativistic vacuum variable q. Here, a cosmological nonequilibrium context is considered with a corresponding time-dependent cosmological parameter \Lambda(t) or vacuum energy density \rho_V(t). A specific model of a closed Friedmann-Robertson-Walker universe is presented, which is determined by equilibrium boundary conditions at one instant of time (t=t_{eq}) and a particular form of vacuum-energy dynamics (d\rho_V/dt \propto \rho_M). This homogeneous and isotropic model has a standard Big Bang phase at early times (t << t_{eq}) and reproduces the main characteristics of the present universe (t=t_0 < t_{eq}).

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