Fischler-Susskind holographic cosmology revisited
arXiv:0704.1637 · doi:10.1088/0264-9381/24/22/019
Abstract
When Fischler and Susskind proposed a holographic prescription based on the Particle Horizon, they found that spatially closed cosmological models do not verify it due to the apparently unavoidable recontraction of the Particle Horizon area. In this article, after a short review of their original work, we expose graphically and analytically that spatially closed cosmological models can avoid this problem if they expand fast enough. It has been also shown that the Holographic Principle is saturated for a codimension one brane dominated Universe. The Fischler-Susskind prescription is used to obtain the maximum number of degrees of freedom per Planck volume at the Planck era compatible with the Holographic Principle.
arXiv comment17 pages, 4 figures. A new example developed in subsection 3.3 and other minor changes
References in corpus (21)
- The Large N Limit of Superconformal Field Theories and Supergravity
- Type Ia Supernova Discoveries at z>1 From the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution
- The World as a Hologram
- Cosmological parameters from SDSS and WMAP
- A Model of Holographic Dark Energy
- The holographic principle
- Entropy Bounds and Dark Energy
- Holography in General Space-times
- Interacting holographic dark energy model in non-flat universe
- Holography, Cosmology and the Second Law of Thermodynamics
- Minimal conditions for the creation of a Friedman-Robertson-Walker universe from a "bounce"
- Cosmology vs. Holography
- Prospects of Inflation
- Remarks on Tachyon Driven Cosmology
- Holographic Cosmology 3.0
- Holographic Principle in the Closed Universe : a Resolution with Negative Pressure Matter
- Observational Constraints On Power-Law Cosmologies
- Relaxing to Three Dimensions
- Closed universes can satisfy the holographic principle in three dimensions
- A Note on Thermodynamics and Holography of Moving Giant Gravitons
- Encoding the scaling of the cosmological variables with the Euler Beta function