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Cosmology vs. Holography
High Energy Physics - Theory · Submitted 19 Apr 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These constraints do not allow one to rule out closed universes and other universes which may experience gravitational collapse, and do not impose any constraints on inflationary cosmology.
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The abstract, sentence by sentence
The most radical version of the holographic principle asserts that all information about physical processes in the world can be stored on its surface. This formulation is at odds with inflationary cosmology, which implies that physical processes in our part of the universe do not depend on the boundary conditions. Also, there are some indications that the radical version of the holographic theory in the context of cosmology may have problems with unitarity and causality. Another formulation of the holographic principle, due to Fischler and Susskind, implies that the entropy of matter inside the post-inflationary particle horizon must be smaller than the area of the horizon. Their conjecture was very successful for a wide class of open and flat universes, but it did not apply to closed universes. Bak and Rey proposed a different holographic bound on entropy which was valid for closed universes of a certain type. However, as we will show, neither proposal applies to open, flat and closed universes with matter and a small negative cosmological constant. We will argue, in agreement with Easther, Lowe, and Veneziano, that whenever the holographic constraint on the entropy inside the horizon is valid, it follows from the Bekenstein-Hawking bound on the black hole entropy. These constraints do not allow one to rule out closed universes and other universes which may experience gravitational collapse, and do not impose any constraints on inflationary cosmology.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The most radical version of the holographic principle asserts that all information about physical processes in the world can be stored on its surface. | background 1.00 | 0.03 | 0.02 | asserted 0.98 |
| s1 | This formulation is at odds with inflationary cosmology, which implies that physical processes in our part of the universe do not depend on the boundary conditions. | background 0.99 | 0.05 | 0.05 | asserted 0.97 |
| s2 | Also, there are some indications that the radical version of the holographic theory in the context of cosmology may have problems with unitarity and causality. | background 0.98 | 0.07 | 0.04 | hedged possibility 1.00 |
| s3 | Another formulation of the holographic principle, due to Fischler and Susskind, implies that the entropy of matter inside the post-inflationary particle horizon must be smaller than the area of the horizon. | background 1.00 | 0.03 | 0.04 | asserted 0.96 |
| s4 | Their conjecture was very successful for a wide class of open and flat universes, but it did not apply to closed universes. | background 0.94 | 0.04 | 0.03 | asserted 1.00 |
| s5 | Bak and Rey proposed a different holographic bound on entropy which was valid for closed universes of a certain type. | background 0.99 | 0.04 | 0.03 | asserted 1.00 |
| s6 | However, as we will show, neither proposal applies to open, flat and closed universes with matter and a small negative cosmological constant. | result 0.83 | 0.80 | 0.32 | asserted 1.00 |
| s7 | We will argue, in agreement with Easther, Lowe, and Veneziano, that whenever the holographic constraint on the entropy inside the horizon is valid, it follows from the Bekenstein-Hawking bound on the black hole entropy. | result 0.52 | 0.35 | 0.44 | asserted 0.94 |
| s8 | These constraints do not allow one to rule out closed universes and other universes which may experience gravitational collapse, and do not impose any constraints on inflationary cosmology. | interpretation 0.79 | 0.63 | 0.67 | asserted 1.00 |
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Original abstract
The most radical version of the holographic principle asserts that all information about physical processes in the world can be stored on its surface. This formulation is at odds with inflationary cosmology, which implies that physical processes in our part of the universe do not depend on the boundary conditions. Also, there are some indications that the radical version of the holographic theory in the context of cosmology may have problems with unitarity and causality. Another formulation of the holographic principle, due to Fischler and Susskind, implies that the entropy of matter inside the post-inflationary particle horizon must be smaller than the area of the horizon. Their conjecture was very successful for a wide class of open and flat universes, but it did not apply to closed universes. Bak and Rey proposed a different holographic bound on entropy which was valid for closed universes of a certain type. However, as we will show, neither proposal applies to open, flat and closed universes with matter and a small negative cosmological constant. We will argue, in agreement with Easther, Lowe, and Veneziano, that whenever the holographic constraint on the entropy inside the horizon is valid, it follows from the Bekenstein-Hawking bound on the black hole entropy. These constraints do not allow one to rule out closed universes and other universes which may experience gravitational collapse, and do not impose any constraints on inflationary cosmology.
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References
How the literature uses it
7 arXiv papers cite this in 12 sentences
Papers citing it · 8 sentences without a confident label
Contests it 1 paper
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The latter choice—called a “covariant bound” in Refs. [ref] but related to [ref] and distinct from [ref] —is excluded by a counterexample [ref] and would not lead to a valid Generalized Second Law.] And finally, it is not immediately obvious that an area law can hold once timelike and spacelike portions are considered together.
Proof of a New Area Law in General Relativity · Introduction · contest 0.72
Compares with it 1 paper
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In Refs. [ref] , the cutoff time is introduced because of the curvature singularity.
Entropy Bound and a Geometrically Nonsingular Universe · Our criterion for the cutoff time · 0.89
Cites it as background 2 papers
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The applications of the holographic principle to cosmology was first carried out by Fischler and Susskind [ref] , and in the past decades had been extensively studied [ref] .
Stephani Cosmology: Entropically Viable But Observationally Challenged · Introduction: Inhomogeneous Cosmologies and Their Constraints · 1.00
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See also Refs. [ref] for discussion on the entropy bound in the universe including accelerating one.
Entropy Bound and a Geometrically Nonsingular Universe · Introduction · 0.82
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