Models of universe with a polytropic equation of state: I. The early universe

Abstract

We construct models of universe with a generalized equation of state $p=(\alpha \rho +k{\rho }^{1+1/n})c^2$ having a linear component and a polytropic component. In this paper, we consider positive indices $n>0$. In that case, the polytropic component dominates in the early universe where the density is high. For $\alpha =1/3$, $n=1$ and $k=-4/(3{\rho }_P)$, we obtain a model of early universe describing the transition from a pre-radiation era to the radiation era. The universe exists at any time in the past and there is no singularity. However, for $t<0$, its size is less than the Planck length $l_P=1.6210^{-35}m$. In this model, the universe undergoes an inflationary expansion with the Planck density ${\rho }_P=5.1610^{99}g/m^3$ that brings it to a size $a_1=2.6110^{-6}m$ at $t_1=1.2510^{-42}s$ (about 20 Planck times $t_P$). For $\alpha =1/3$, $n=1$ and $k=4/(3{\rho }_P)$, we obtain a model of early universe with a new form of primordial singularity: The universe starts at t=0 with an infinite density and a finite radius $a=a_1$. Actually, this universe becomes physical at a time $t_i=8.3210^{-45}s$ from which the velocity of sound is less than the speed of light. When $a\gg a_1$, the universe evolves like in the standard model. We describe the transition from the pre-radiation era to the radiation era by analogy with a second order phase transition where the Planck constant $\hslash$ plays the role of finite size effects (the standard Big Bang theory is recovered for $\hslash =0$).

References in corpus (1)

• The Cosmological Constant

Cited by in corpus (2)

• Dark Energy: The Shadowy Reflection of Dark Matter?
• Primordial Universe with radiation and Bose-Einstein condensate