Holographic calculation of BMSFT mutual and 3-partite information

Asadi, Mohsen; Fareghbal, Reza

doi:10.1140/epjc/s10052-018-6098-0

Cited by 9 publications

(4 citation statements)

References 38 publications

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“…By using the coordinate transformations 15) we can change the metric of null-orbifold to the Cartesian coordinate…”

Section: Holographic Entanglement Entropy In Flat/bmsftmentioning

confidence: 99%

“…This situation is very similar to the two-dimensional conformal field theories (CFTs) which their infinite-dimensional symmetry is used to predict the structure of correlation functions as well as entanglement entropy of subsystems. Similarly, the entanglement entropy formula for some particular intervals in BMSFT 2 has been introduced in [8] by just using the infinite symmetry of two-dimensional BMSFTs and then studied more carefully in [9]- [15].…”

Section: Introductionmentioning

confidence: 99%

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First law of entanglement entropy in flat-space holography

Fareghbal

Shalamzari

2019

Phys. Rev. D

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According to flat/Bondi-Metzner-Sachs invariant field theories (BMSFT) correspondence, asymptotically flat spacetimes in (d + 1)-dimensions are dual to d-dimensional BMSFTs. In this duality, similar to the Ryu-Takayanagi proposal in the AdS/CFT correspondence, the entanglement entropy of subsystems in the field theory side is given by the area of some particular surfaces in the gravity side. In this paper we find the holographic counterpart of the first law of entanglement entropy (FLEE) in a two-dimensional BMSFT. We show that FLEE for the BMSFT perturbed states which are descried by three-dimensional flat-space cosmology, corresponds to the integral of a particular one-form on a closed curve. This curve consists of BMSFT interval and also null and spacelike geodesics in the bulk gravitational theory. Exterior derivative of this form is zero when it is calculated for the flat-space cosmology. However, for a generic perturbation of three-dimensional global Minkowski spacetime, the exterior derivative of one-form yields Einstein equation. This is the first step for constructing bulk geometry by using FLEE in the flat/BMSFT correspondence.

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“…By using the coordinate transformations 15) we can change the metric of null-orbifold to the Cartesian coordinate…”

Section: Holographic Entanglement Entropy In Flat/bmsftmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

First law of entanglement entropy in flat-space holography

Fareghbal

Shalamzari

2019

Phys. Rev. D

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“…For example, in 3-dimensional flat space, the endpoints of E A are in the bulk and connected to ∂A ± by two null geodesics γ ± normal to E A [10]. Recent works related to this geometric picture can be found in [41][42][43]. This new geometric picture of entanglement entropy with the extra null geodesics γ ± is reformulated in [41] following the HRT covariant formulation [7].…”

Section: Introductionmentioning

confidence: 99%

Towards the generalized gravitational entropy for spacetimes with non-Lorentz invariant duals

Wen

2019

J. High Energ. Phys.

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Based on the Lewkowycz-Maldacena prescription and the fine structure analysis of holographic entanglement proposed in [1], we explicitly calculate the holographic entanglement entropy for warped CFT that duals to AdS 3 with a Dirichlet-Neumann type of boundary conditions. We find that certain type of null geodesics emanating from the entangling surface ∂A relate the field theory UV cutoff and the gravity IR cutoff. Inspired by the construction, we furthermore propose an intrinsic prescription to calculate the generalized gravitational entropy for general spacetimes with non-Lorentz invariant duals. Compared with the RT formula, there are two main differences. Firstly, instead of requiring that the bulk extremal surface E should be anchored on ∂A, we require the consistency between the boundary and bulk causal structures to determine the corresponding E. Secondly we use the null geodesics (or hypersurfaces) emanating from ∂A and normal to E to regulate E in the bulk. We apply this prescription to flat space in three dimensions and get the entanglement entropies straightforwardly. arXiv:1810.11756v3 [hep-th] 29 Jan 20191 The extremal condition is the result of imposing the equations of motion and replica symmetry on all the fields in the action. In [13], as the gauge fields are nondynamical and do not appear in the symplectic structure, thus should not be imposed with the replica symmetry (or periodic) condition. As a result, in that case the geometric quantity E that measures the entanglement entropy is not an extremal surface. See [14] for a simpler discussion on the extremal condition.2 A proof for the homology constraint at topological level in AdS/CFT is given in [19] 3 Although the AdS/CFT has attracted most of the attentions, the holographic principle is assumed to be hold for general spacetimes. So far the holography beyond AdS/CFT that has been proposed include the dS/CFT correspondence [20], the Lifshitz spacetime/Lifshitz-type field theory duality [21][22][23][24], the Kerr/CFT correspondence [25], the WAdS/CFT [26,27] or WAdS/WCFT [28,29] correspondence, and flat holography in four dimensions [30][31][32] and three dimensions [33][34][35].

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“…The universal structure of the correlation functions of BMSFT 2 and BMSFT 3 has been studied in [9][10][11][12]. The entanglement entropy formula and also the holographic interpretation of this formula in the context of flat/BMSFT have been studied in [13][14][15][16][17][18][19][20]. In all of the above mentioned works, the calculations that are done in asymptotically flat spacetimes nicely fit to the results given by taking the ultrarelativistic limit of CFTs.…”

Section: Introductionmentioning

confidence: 77%

Complexity growth in flat spacetimes

Fareghbal

Karimi

2018

Phys. Rev. D

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We use the complexity equals action proposal to calculate the rate of complexity growth for field theories that are the holographic duals of asymptotically flat spacetimes. To this aim, we evaluate the on-shell action of asymptotically flat spacetime on the Wheeler-DeWitt patch. This results in the same expression as can be found by taking the flat-space limit from the corresponding formula related to the asymptotically AdS spacetimes. For the bulk dimensions that are greater than three, the rate of complexity growth at late times approaches from above to Lloyd's bound. However, for the three-dimensional bulks, this rate is a constant and differs from Lloyd's bound by a logarithmic term.

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Holographic calculation of BMSFT mutual and 3-partite information

Cited by 9 publications

References 38 publications

First law of entanglement entropy in flat-space holography

First law of entanglement entropy in flat-space holography

Towards the generalized gravitational entropy for spacetimes with non-Lorentz invariant duals

Complexity growth in flat spacetimes

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