Holographic equipartition and the maximization of entropy

Krishna, P. B.; Mathew, Titus K.

doi:10.1103/physrevd.96.063513

Cited by 42 publications

(46 citation statements)

References 23 publications

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“…Can the expansion of the universe toward a quiescent de Sitter phase be interpreted as thermodynamic equilibration to a maximum-entropy state? It is well established that de Sitter has many of the properties of an equilibrium maximum-entropy state, including a locally thermal density matrix with a constant temperature [21,22], and the relationship between entropy and de Sitter space has been examined from a variety of perspectives [23][24][25][26][27][28][29][30][31].…”

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confidence: 99%

Cosmic equilibration: A holographic no-hair theorem from the generalized second law

Carroll

Chatwin-Davies

2018

Phys. Rev. D

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In a wide class of cosmological models, a positive cosmological constant drives cosmological evolution toward an asymptotically de Sitter phase. Here we connect this behavior to the increase of entropy over time, based on the idea that de Sitter spacetime is a maximum-entropy state. We prove a cosmic no-hair theorem for Robertson-Walker and Bianchi I spacetimes that admit a Q-screen ("quantum" holographic screen) with certain entropic properties: If generalized entropy, in the sense of the cosmological version of the generalized second law conjectured by Bousso and Engelhardt, increases up to a finite maximum value along the screen, then the spacetime is asymptotically de Sitter in the future. Moreover, the limiting value of generalized entropy coincides with the de Sitter horizon entropy. We do not use the Einstein field equations in our proof, nor do we assume the existence of a positive cosmological constant. As such, asymptotic relaxation to a de Sitter phase can, in a precise sense, be thought of as cosmological equilibration.

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confidence: 99%

Cosmic equilibration: A holographic no-hair theorem from the generalized second law

Carroll

Chatwin-Davies

2018

Phys. Rev. D

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“…The Hubble horizon of a de Sitter universe is equivalent to an apparent horizon because the universe is spatially flat. For the thermodynamics of de Sitter universes, see previous works [59][60][61][62][63][64].…”

Section: Horizon Thermodynamics and Holographic Equipartition Lawmentioning

confidence: 99%

“…In addition, the thermodynamics of the Universe has been studied from various viewpoints . In particular, the maximization of entropy has been investigated recently [51][52][53][59][60][61][62][63][64][65], and these studies suggest that our Universe should approach a Λ-dominated universe, namely a de Sitter universe, at least in the last stage, as if our Universe behaves as an ordinary macroscopic system [59]. A de Sitter universe is considered to be in thermal equilibrium based on horizon thermodynamics.…”

Section: Introductionmentioning

confidence: 99%

Energy stored on a cosmological horizon and its thermodynamic fluctuations in holographic equipartition law

Komatsu

2021

Preprint

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Our Universe is expected to finally approach a de Sitter universe whose horizon is considered to be in thermal equilibrium. In the present article, both the energy stored on the horizon and its thermodynamic fluctuations are examined through the holographic equipartition law. First, it is confirmed that a flat Friedmann-Robertson-Walker universe approaches a de Sitter universe, using a cosmological model close to lambda cold dark matter (ΛCDM) models. Then, based on the holographic equipartition law, the energy density of the Hubble volume is calculated from the energy on the Hubble horizon of a de Sitter universe. The energy density for a de Sitter universe is constant and the order of the energy density is consistent with the order of that for the observed cosmological constant. Second, thermodynamic fluctuations of energy on the horizon are examined, assuming stable fluctuations around thermal equilibrium states. A standard formulation of the fluctuations for a canonical ensemble is applied to the Hubble horizon of a de Sitter universe. The thermodynamic fluctuations of the energy are found to be a universal constant corresponding to the Planck energy, regardless of the Hubble parameter. In contrast, the relative fluctuations of the energy can be characterized by the ratio of the one-degree-of-freedom energy to the Planck energy. At the present time, the order of the relative fluctuations should be within the range of a discrepancy derived from a discussion of the cosmological constant problem, namely a range approximately from 10 −60 to 10 −123 . The present results may imply that the energy stored on the Hubble horizon is related to a kind of effective dark energy, whereas the energy that can be 'maximumly' stored on the horizon may behave as if it were a kind of effective vacuum-like energy in an extended holographic equipartition law.

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“…In [26] we had suggested that the convenient physical parameter to measure information (or entropy), instead of mass or energy, is the action that usually is considered to be additive like entropy and have a unique discrete value, . In this approach, the maximal entropy (minimal information) principle [37][38][39], is equivalent to the familiar minimal action principle. However, the minimal information principle is more general, especially for quantum descriptions, since in physical equations one can introduce the information entropy terms that correspond to measurement processes.…”

Section: Information-probabilistic Ideamentioning

confidence: 99%

Information-Probabilistic Description of the Universe

Gogberashvili

2016

Int J Theor Phys

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We describe the universe as a single entangled ensemble of quantum particles. The total entropy of this world ensemble, which can be expressed as a sum of information, thermodynamic and entanglement components, is assumed to be always zero. This condition suggests information quantization, which we associate with the Planck's action. Then the entropy neutrality condition for the universe leads to the zero-action principle. We show that the main concepts of classical space-time and gravity naturally emerge in this picture. A generalized least action principle, which embraces the maximal entropy principles of information theory, is introduced.

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Holographic equipartition and the maximization of entropy

Cited by 42 publications

References 23 publications

Cosmic equilibration: A holographic no-hair theorem from the generalized second law

Cosmic equilibration: A holographic no-hair theorem from the generalized second law

Energy stored on a cosmological horizon and its thermodynamic fluctuations in holographic equipartition law

Information-Probabilistic Description of the Universe

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