Random vs. holographic fluctuations of the background metric. II. Note on the dark energies arising due to microstructure of space-time
Andronikashvili Institute of Physics - 6 Tamarashvili St., Tbilisi 0177, Georgia and Center for Elementary Particle Physics, ITP, Ilia State University - 3–5 Cholokashvili Ave., Tbilisi 0162, Georgia
Accepted: 22 July 2010
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.
PACS: 04.60.-m – Quantum gravity / 04.60.Bc – Phenomenology of quantum gravity
© EPLA, 2010