Entanglement entropy in de Sitter space

Maldacena, Juan; Pimentel, Guilherme L.

doi:10.1007/jhep02(2013)038

Cited by 169 publications

(261 citation statements)

References 67 publications

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“…This agrees with [29] who derived it from a late time RT surface, as it must, since the RT method agrees with the CHM method for arbitrary size spherical entangling regions, as we show in appendix A. Ref. [30] also computed the holographic RT surfaces that measure the EE of a spherical region in a CFT in de Sitter space in various dimensions.…”

Section: Jhep03(2016)172supporting

confidence: 84%

“…We emphasise that the EE of superhorizon sized regions probes the FRW geometry behind the horizon of the de Sitter slicing of AdS, as noted in [29]. Reference [30] argued that the EE of superhorizon sized regions is given by an expression different from (3.18) and concluded that the EE goes through a phase transition when R crosses the horizon.…”

Section: Cft Entanglement Entropy From Chm Mapmentioning

confidence: 80%

“…Specialising now to 4d field theories in de Sitter, an important limit is when the entangling sphere is much bigger than the de Sitter horizon, R/l 1. In this case the overall finite part of the EE of a spherical region in dS 4 is expected to follow [29] S finite = a 5 R 2 l 2 + a 6 ln (R/l) + +subleading, (2.5) where the coefficient of the log term contains information about the long range entanglement of the state, related to particle creation effects in de Sitter. This term is not present in flat space.…”

Section: Jhep03(2016)172mentioning

confidence: 99%

“…For a CFT a 6 = −a 2 . Reference [29] further argued that when the mass scale of the relevant operator is small (compared to H), there is a non-zero a 6 , whereas when the mass scale is large, or the…”

Section: Jhep03(2016)172mentioning

confidence: 99%

“…For holographic theories on de Sitter the idea is that when the dual bulk geometry is ungapped, it contains another region that can be accessed by analytically continuing through a bulk horizon, whose metric is that of an expanding and contracting FRW cosmology. Extremal surfaces measuring the EE of superhorizon sized regions in de Sitter probe this FRW part of the bulk, and in the limit R l the surfaces lies along the slice of maximal FRW scale factor, which gives a non-zero coefficient a 6 [29].…”

Section: Jhep03(2016)172mentioning

confidence: 99%

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Holographic entanglement entropy for massive flavours in dS 4

Vaganov

2016

J. High Energ. Phys.

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We examine the holographic entanglement entropy of spherical regions in de Sitter space in the presence of massive flavour fields which are modelled by probe D7 branes in AdS 5 × S 5 . We focus on the finite part of the massive correction to the entropy in the limits of small mass and large mass that are separated by a phase transition between two topologically distinct brane embeddings. For small masses, it approaches the flat space result for small spheres, whereas for large spheres there is a term that goes as the log of the sphere radius. For large masses, we find evidence for a universal contribution logarithmic in the mass. In all cases the entanglement entropy is smooth as the sphere radius crosses the horizon.

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Section: Jhep03(2016)172supporting

confidence: 84%

Section: Cft Entanglement Entropy From Chm Mapmentioning

confidence: 80%

Section: Jhep03(2016)172mentioning

confidence: 99%

Section: Jhep03(2016)172mentioning

confidence: 99%

Section: Jhep03(2016)172mentioning

confidence: 99%

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Holographic entanglement entropy for massive flavours in dS 4

Vaganov

2016

J. High Energ. Phys.

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Distribution and Generation of Quantum Coherence for Gaussian States in de Sitter Space

et al. 2021

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The distribution and generation of quantum coherence for two‐mode and multi‐mode Gaussian states in de Sitter space are studied. It is found that the quantum coherence is redistributed among the mode in different open charts under the curvature effect of de Sitter space. In particular, the Gaussian coherence for the initially correlated state is found to survive in the limit of infinite curvature, while quantum entanglement vanishes in this limit. Unlike entanglement and steering, the coherence of a massive scalar field is more robust than a massless field under the influence of curvature of de Sitter space. In addition, it is shown that the curvature generates two‐mode Gaussian state and three‐mode Gaussian state quantum coherence among the open charts, even though the observers are localized in causally disconnected regions. It is worth noting that the gravity‐generated three‐mode coherence is extremely sensitive to the curvature effect for the conformal and massless scalar fields, which may be in principle employed to design an effective detector for the space curvature.

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C${\cal C}$osmological G${\cal G}$eometric P${\cal P}$hase F${\cal F}$rom P${\cal P}$ure Q${\cal Q}$uantum S${\cal S}$tates: A Study without/ with having Bell's Inequality Violation

Choudhury

2022

Fortschritte der Physik

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In this paper, using the concept of Lewis Riesenfeld invariant quantum operator method for finding continuous eigenvalues of quantum mechanical wave functions we derive the analytical expressions for the cosmological geometric phase, which is commonly identified to be the Pancharatnam Berry phase from primordial cosmological perturbation scenario. We compute this cosmological geometric phase from two possible physical situations, (1) In the absence of Bell's inequality violation and (2) In the presence of Bell's inequality violation having the contributions in the sub Hubble region (−kτ≫1$-k\tau \gg 1$), super Hubble region (−kτ≪1$-k\tau \ll 1$) and at the horizon crossing point (−kτ=1$-k\tau = 1$) for massless field (m/scriptH≪1$m/{\cal H}\ll 1$), partially massless field (m/scriptH∼1$m/{\cal H}\sim 1$) and massive/heavy field (m/scriptH≫1$m/{\cal H}\gg 1$), in the background of quantum field theory of spatially flat quasi De Sitter geometry. The prime motivation for this work is to investigate the various unknown quantum mechanical features of primordial universe. To give the realistic interpretation of the derived theoretical results we express everything initially in terms of slowly varying conformal time dependent parameters, and then to connect with cosmological observation we further express the results in terms of cosmological observables, which are spectral index/tilt of scalar mode power spectrum (nζ$n_{\zeta }$) and tensor‐to‐scalar ratio (r). Finally, this identification helps us to provide the stringent numerical constraints on the Pancharatnam Berry phase, which confronts well with recent cosmological observation.

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Entanglement entropy in de Sitter space

Cited by 169 publications

References 67 publications

Holographic entanglement entropy for massive flavours in dS 4

Holographic entanglement entropy for massive flavours in dS 4

Distribution and Generation of Quantum Coherence for Gaussian States in de Sitter Space

C${\cal C}$osmological G${\cal G}$eometric P${\cal P}$hase F${\cal F}$rom P${\cal P}$ure Q${\cal Q}$uantum S${\cal S}$tates: A Study without/ with having Bell's Inequality Violation

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