No Page curves for the de Sitter horizon

Kames-King, Joshua; Verheijden, Evita; Verlinde, Erik

doi:10.1007/jhep03(2022)040

Cited by 38 publications

(27 citation statements)

References 65 publications

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“…Nonetheless, it would be interesting to see what one could glean from the Wald entropy associated with the anomaly induced action for fourdimensional general relativity. Finally, our results reasonably apply in equilibrium settings, and therefore we cannot comment on Page curves in dynamical backgrounds, including the dS 2 scenarios described in [23,24,46,47]. It would be interesting to see whether one can express the dynamical black hole entropy proposal of [77] as a "microcanonical" action, and apply it to diamonds.…”

Section: Discussionmentioning

confidence: 84%

“…In cosmology one encounters a puzzle similar to the black hole information paradox, such that fine grained matter entropies violate the Bekenstein entropy bound [41] (see also [42]). Consequently, the QES and island formulae (1.4) have been employed to analyze fine grained entropies in de Sitter space in different settings [23,24,[43][44][45][46][47], e.g., in the full or half reduction model, and for radiation collected inside the static patch or at future infinity. Most relevant to our discussion here is the distinction between the full and half reduction model of de Sitter JT gravity.…”

Section: Below)mentioning

confidence: 99%

“…Here we summarize various useful coordinates to describe two-dimensional de Sitter space (see also [46,61,102]).…”

Section: Coordinate Systemsmentioning

confidence: 99%

See 2 more Smart Citations

Quasi-local energy and microcanonical entropy in two-dimensional nearly de Sitter gravity

Svesko¹,

Verheijden²,

Verlinde³

et al. 2022

Preprint

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We study the semi-classical thermodynamics of two-dimensional de Sitter space (dS 2 ) in Jackiw-Teitelboim (JT) gravity coupled to conformal matter. We extend the quasilocal formalism of Brown and York to dS 2 , where a timelike boundary is introduced in the static patch to uniquely define conserved charges, including quasi-local energy. The boundary divides the static patch into two systems, a cosmological system and a black hole system, the former being unstable under thermal fluctuations while the latter is stable. A semi-classical quasi-local first law is derived, where the Gibbons-Hawking entropy is replaced by the generalized entropy. In the microcanonical ensemble the generalized entropy is stationary. Further, we show the on-shell Euclidean microcanonical action of a causal diamond in semi-classical JT gravity equals minus the generalized entropy of the diamond, hence extremization of the entropy follows from minimizing the action. Thus, we provide a first principles derivation of the island rule for U (1) symmetric dS 2 backgrounds, without invoking the replica trick. We discuss the implications of our findings for static patch de Sitter holography.

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Section: Discussionmentioning

confidence: 84%

Section: Below)mentioning

confidence: 99%

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Quasi-local energy and microcanonical entropy in two-dimensional nearly de Sitter gravity

Svesko¹,

Verheijden²,

Verlinde³

et al. 2022

Preprint

Self Cite

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show abstract

“…These include space-time connections between the bra and ket of the wave function of the universe [213], as well as the appearance of 'islands' in the calculation of entropy in various regions of the inflating universe: see e.g. [213][214][215][216][217][218][219][220].…”

Section: Initial Conditions Semiclassicallymentioning

confidence: 99%

Snowmass White Paper: Cosmology at the Theory Frontier

Flauger¹,

Gorbenko²,

Joyce³

et al. 2022

Preprint

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The precision cosmological model describing the origin and expansion history of the universe, with observed structure seeded at the inflationary cosmic horizon, demands completion in the ultraviolet and in the infrared. The dynamics of the cosmic horizon also suggests an associated entropy, again requiring a microphysical theory. Recent years have seen enormous progress in understanding the structure of de Sitter space and inflation in string theory, and of cosmological observables captured by quantum field theory and solvable deformations thereof. The resulting models admit ongoing observational tests through measurements of the cosmic microwave background and large-scale structure, as well as through analyses of theoretical consistency by means of thought experiments. This paper, prepared for the TF01 and TF09 conveners of the Snowmass 2021 process, provides a synopsis of this important area, focusing on ongoing developments and opportunities.

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“…In this paper, we consider entanglement entropy in cosmological spacetimes and study the lessons from the finiteness of Hilbert space dimension in gravity, using the entanglement island. The entanglement islands in various cosmological spacetimes have been studied in [39,40,[64][65][66][67][68][69][70][71]. From the holographic principle and the extension of Bekenstein bound to cosmological spacetimes, the entropy of a region A of a time slice is upper bounded by its boundary area [72][73][74][75][76][77][78]…”

Section: Introductionmentioning

confidence: 99%

Island for Gravitationally Prepared State and Pseudo Entanglement Wedge

Miyaji

2021

Preprint

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We consider spacetime initiated by a finite-sized boundary on which a pure initial matter state is set as a natural generalization of the Hartle-Hawking noboundary state. We study entanglement entropy of the gravitationally prepared matter state at the final time slice. We find that the entropy of the initial state or the entanglement island gives the entropy for large subregions on the final time slice. Consequently, we find the entanglement entropy is bounded from above by the boundary area of the island, leading to an entropy bound in terms of the island formula. The island I appears in the analytically continued spacetime, either at the bra or the ket part of the spacetime in Schwinger-Keldysh formalism, and the entropy is given by an average of pseudo entropy of each entanglement island. We find a necessary condition of the initial state to be consistent with the strong subadditivity. The condition requires that any probe degrees of freedom are thermally entangled with the rest of the system. We then study which initial condition leads to our finite-sized initial boundary or the Hartle-Hawking no-boundary state. Due to the absence of a moment of time reflection symmetry, the island in our setup requires a generalization of the entanglement wedge, which we call pseudo entanglement wedge. In pseudo entanglement wedge reconstruction, we consider reconstructing the bulk matter transition matrix on A ∪ I, from a fine-grained state on A. The bulk transition matrix is given by a thermofield double state with a projection by the initial state. We provide an AdS/BCFT model, which provides a double holography model of our setup by considering EOW branes with corners. We also find the exponential hardness of such reconstruction task using a generalization of Python's lunch conjecture to pseudo generalized entropy.

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No Page curves for the de Sitter horizon

Cited by 38 publications

References 65 publications

Quasi-local energy and microcanonical entropy in two-dimensional nearly de Sitter gravity

Quasi-local energy and microcanonical entropy in two-dimensional nearly de Sitter gravity

Snowmass White Paper: Cosmology at the Theory Frontier

Island for Gravitationally Prepared State and Pseudo Entanglement Wedge

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