Black Holes in the Turbulent Phase of Viscous Rip Cosmology

Iver Brevik; Mubasher Jamil

doi:10.1142/S0219887819500300

paper

Black Holes in the Turbulent Phase of Viscous Rip Cosmology

arXiv:1901.00002 · doi:10.1142/S0219887819500300

Abstract

We study the phantom fluid in the late universe, thus assuming the equation of state parameter $w$ to be less than $- 1$ . The fluid is assumed to consist of two components, one laminar component $ρ$ and one turbulent component $ρ_{T}$ , the latter set proportional to $ρ$ as well as to the Hubble parameter, $ρ_{T} = 3 τ H ρ$ with $τ$ a positive constant associated with the turbulence. The effective energy density is taken to be $ρ_{e} = ρ + ρ_{T}$ , and the corresponding effective pressure is $p_{e} = w ρ_{e}$ , with $w$ constant. These basic assumptions lead to a Big Rip universe; the physical quantities diverging during a finite rip time $t_{s}$ . We then consider the mass accretion of a black hole in such a universe. The most natural assumption of setting the rate $d M / d t$ proportional to $M^{2}$ times the sum $ρ_{e} + p_{e}$ , leads to a negative mass accretion, where $M (t)$ goes to zero linearly in $(t_{s} - t)$ near the singularity. The Hubble parameter diverges as $(t_{s} - t)^{- 1}$ , whereas $ρ_{e}$ and $p_{e}$ diverge as $(t_{s} - t)^{- 2}$ . We also discuss other options and include, for the sake of comparison, some essential properties of mass accretion in the early (inflationary) universe.

arXiv comment7 pages latex 2e, no figures; to appear in Int. J. Geom. Meth. Mod. Phys

Black Holes in the Turbulent Phase of Viscous Rip Cosmology

Abstract

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