Dark Energy and Cosmological Horizon Thermal Effects

Abstract

We investigate various dark energy models by taking into account the thermal effects induced from Hawking radiation on the apparent horizon of the Universe, for example near a finite-time future singularity. If the dark energy density increases as the Universe expands, the Universe's evolution reaches a singularity of II type (or sudden future singularity). The second derivative of scale factor diverges but the first remains finite. Quasi-de Sitter evolution can change on sudden future singularity in the case of having an effective cosmological constant larger than the maximum possible value of the energy density of the Universe. Another interesting feature of cosmological solution is the possibility of a transition between deceleration and acceleration for quintessence dark energy with a simple equation of state. Finally, we investigate which fluid component can remedy Big Rip singularities and other crushing type singularities.

15 pp., 7 figs., to appear in Phys. Rev. D

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Cited by in corpus (5)

• Energy conditions for Inhomogeneous EOS and its Thermodynamics analysis with the resolution on finite time future singularity problems
• Singular behavior of the dark universe under the effect of thermal radiation in curved spacetime
• Observational Constraints on Chaplygin Gas Models in Non-Minimally Coupled Power Law $f(Q)$ Gravity with Quasars
• Magnetic black hole in Einstein-Dilaton-Square root nonlinear electrodynamics
• Singularity softening and avoidance by the action of thermal radiation in a generalized entropic cosmology