Positive vacuum energy and the N-bound

By R. Bousso. 2000

264 citations recorded by the source corpus.

We argue that the total observable entropy is bounded by the inverse of the cosmological constant. This holds for all space-times with a positive cosmological constant, including cosmologies dominated by ordinary matter, and recollapsing universes. The argument involves intermediate steps which may be of interest in their own right. We note that entropy cannot be observed unless it lies both in the past and in the future of the observer's history. This truncates space-time to a diamond-shaped subset well-suited to the application of the covariant entropy bound. We further require, and derive, a novel Bekenstein-like bound on matter entropy in asymptotically de Sitter spaces. Our main result lends support to the proposal that universes with positive cosmological constant are described by a fundamental theory with only a finite number of degrees of freedom.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/50f028089d752c60387d3c86c1f5031867c7853a

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Citations in the corpus

The trouble with de Sitter space (2002, background): “Thus far the holographic principle [2, 3, 4] has not produced a dual description of de Sitter space analogous to the holographic duality between anti–de Sitter space and Super Yang Mills theory [5, 6, 7] A number of authors [10, 11, 12, 13, 14, 15, 16, 17, 18] have argued for a de Sitter complementa”
M theory observables for cosmological space-times (2001, background): “At lowest order in α ′ the vertex operators are in one to one correspondence with solutions with given asymptotics on the boundaries of the spacetime, including the Big Bang.”
Disturbing Implications of a Cosmological Constant (2002, unknown): “covariant entropy bound as proposed in [30].”
The dS/CFT Correspondence and the Big Smash (2001, background): “…the CFTs in dS/CFT are of a radically unconventional form, and this opens up the possibility that Smash-free Phantom spacetimes offer a simple model of a “bouncing” cosmology in which the quantum-mechanical entanglement of the field theories in the infinite past and future plays an essential role.”
An algebra of observables for de Sitter space (2022, background): “In the case of de Sitter space, it has been argued that this is not the case: it is claimed that the maximum possible value for Sgen is the value that it has for empty de Sitter space [6, 7, 15].”
Quantum Gravity In De Sitter Space (2001, unknown): “ar X iv :h ep -t h/ 01 06 10 9v 1 1 3 Ju n 20 01 hep-th/0106109 Quantum Gravity In De Sitter Space Edward Witten Dept. of Physics, Cal Tech, Pasadena, CA and”
The Holographic principle (2002, background): “Our construction follows Bousso (1999b); see also Bigatti and Susskind (2000), Bousso (2000a).”
Complementarity is not enough (2012, background): “Causal patches are the fundamental objects of complementarity in arbitrary spacetimes [10], and the covariant entropy bound [11] naturally applies to their boundaries.”
De Sitter Space in Supergravity and M Theory (2001, background): “hy on de Sitter spaces and product spaces. 1. Introduction There has recently been renewed interest in quantum gravity in de Sitter space and the issue of obtaining de Sitter space from string theory [1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11, 12]. Here the ways in which de Sitter space can arise in supergr”
Inflation, holography, and the choice of vacuum in de Sitter space (2002, background): “the point of view of dS/CFT can be found in[48]). The metric in static coordinates is given by ds2 = − 1− H2r2 dt2 + dr2 1− H2r2 +r2dΩ2 d−2, (35) where r < 1/H corresponds to the causaldiamond [70], i.e. the region of space time which the observer can inﬂuence or get inﬂuenced by. If we use pla”
Inflation in AdS/CFT (2005, background): “These constructions do not answer many of the deep questions raised by inflation: How can inflation begin? What measure should be used on the multiverse of eternal inflation? What is the holographic description of inflation? More generally, what degrees of freedom are appropriate for a complete desc”
The dS/CFT correspondence (2001, background): “A second problem recently stressed in [23] is that, if enough matter is present, a space which is asymptotically de Sitter at I− may collapse at finite time, and there will be no future I+ de Sitter region at all.”
Holographic Protection of Chronology in Universes of the Godel Type (2002, background): “[2-6]; see also [7,8] for a complementary point of view on de Sitter holography that uses other preferred screens, not associated with an inertial observer).”