Random versus holographic fluctuations of the background metric. II. Note on the dark energies arising due to microstructure of space-time
arXiv:0901.2402 · doi:10.1209/0295-5075/91/30002
Abstract
Over the last few years a certain class of dark-energy models decaying inversely proportional to the square of the horizon distance emerged on the basis either of Heisenberg uncertainty relations or of the uncertainty relation between the four-volume and the cosmological constant. The very nature of these dark energies is understood to be the same, namely it is the energy of background space/metric fluctuations. Putting together these uncertainty relations one finds that the model of random fluctuations of the background metric is favored over the holographic one.
3 pages
References in corpus (8)
- A Dark Energy Model Characterized by the Age of the Universe
- A New Model of Agegraphic Dark Energy
- Cosmological implications of Karolyhazy uncertainty relation
- Space-time in light of Karolyhazy uncertainty relation
- Is the cosmological "constant" a nonlocal quantum residue of discreteness of the causal set type?
- Space-Time Uncertainty and Approaches to D-Brane Field Theory
- Space-time uncertainty relation and operational definition of dimension
- Random versus holographic fluctuations of the background metric. I. (Cosmological) running of space-time dimension