Black Holes in the Turbulent Phase of Viscous Rip Cosmology

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 $\rho$ and one turbulent component ${\rho }_T$, the latter set proportional to $\rho$ as well as to the Hubble parameter, ${\rho }_T=3\tau H\rho$ with $\tau$ a positive constant associated with the turbulence. The effective energy density is taken to be ${\rho }_e=\rho +{\rho }_T$, and the corresponding effective pressure is $p_e=w{\rho }_e$, 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 $dM/dt$ proportional to $M^2$ times the sum ${\rho }_e+p_e$, 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 ${\rho }_e$ 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.

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

References in corpus (7)

• Viscous Cosmology for Early- and Late-Time Universe
• Turbulence and Little Rip Cosmology
• Characteristic Properties of Two Different Viscous Cosmology Models for the Future Universe
• Generalized second law of thermodynamics for a phantom energy accreting BTZ black hole
• Accretion on Reissner-Nordstrom-(anti)-de Sitter Black Hole with Global Monopole
• Little Rip cosmological models with time-dependent equation of state
• On Isotropic Turbulence in the Dark Fluid Universe

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