Cosmic holographic bounds with UV and IR cutoffs

Details Cosmic holographic bounds with UV and IR cutoffs Cosmic holographic bounds with UV and IR cutoffs

2005-01-05

arxiv.org/abs/hep-th/0501023v1

Mod.Phys.Lett. A20 (2005) 2035

Physics

High Energy Physics

High Energy Physics - Theory

15pages

Scientific paper

10.1142/S0217732305018190

We introduce the cosmic holographic bounds with two UV and IR cutoff scales, to deal with both the inflationary universe in the past and dark energy in the future. To describe quantum fluctuations of inflation on sub-horizon scales, we use the Bekenstein-Hawking energy bound. However, it is not justified that the D-bound is satisfied with the coarse-grained entropy. The Hubble bounds are introduced for classical fluctuations of inflation on super-horizon scales. It turns out that the Hubble entropy bound is satisfied with the entanglement entropy and the Hubble temperature bound leads to a condition for the slow-roll inflation. In order to describe the dark energy, we introduce the holographic energy density which is the one saturating the Bekenstein-Hawking energy bound for a weakly gravitating system. Here the UV (IR) cutoff is given by the Planck scale (future event horizon), respectively. As a result, we find the close connection between quantum and classical fluctuations of inflation, and dark energy.

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