Communication through quantum fields near a black hole

Jonsson, Robert H.; Aruquipa, David Q.; Casals, Marc; Kempf, Achim; Martín-Martínez, Eduardo

doi:10.1103/physrevd.101.125005

Cited by 38 publications

(42 citation statements)

References 63 publications

(154 reference statements)

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“…Another related question concerns the effect of null shockwaves from the perspective of supertranslation [69][70][71]: it would be interesting to study the correlations between two detectors in presence of supertranslations. Finally, it would also be interesting to see how the four vacua considered in this paper affect communication efficiencies such as channel capacities between detectors [72]. We leave these questions for future work.…”

Section: Resultsmentioning

confidence: 95%

“…The most formidable calculations of the two-point functions of this kind are done e.g. in [53,54], though the objectives are different.…”

Section: Jhep08(2020)155mentioning

confidence: 99%

“…Overall, while we do not explore the (extremely vast) parameter space of our setup, the signalling analysis highlights a mechanism through which entanglement harvesting between two detectors at the black hole exterior occurs: the efficiency of the protocol depends strongly on the ability of detectors to signal between them. The very specific issue of quantum communication in (3+1)D Schwarzschild black hole where angular variables of the metric have important role has been very recently investigated using state-of-the-art calculations in [54].…”

Section: Jhep08(2020)155mentioning

confidence: 99%

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Harvesting correlations in Schwarzschild and collapsing shell spacetimes

Tjoa

Mann

2020

J. High Energ. Phys.

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We study the harvesting of correlations by two Unruh-DeWitt static detectors from the vacuum state of a massless scalar field in a background Vaidya spacetime consisting of a collapsing null shell that forms a Schwarzschild black hole (hereafter Vaidya spacetime for brevity), and we compare the results with those associated with the three preferred vacua (Boulware, Unruh, Hartle-Hawking-Israel vacua) of the eternal Schwarzschild black hole spacetime. To do this we make use of the explicit Wightman functions for a massless scalar field available in (1+1)-dimensional models of the collapsing spacetime and Schwarzschild spacetimes, and the detectors couple to the proper time derivative of the field. First we find that, with respect to the harvesting protocol, the Unruh vacuum agrees very well with the Vaidya vacuum near the horizon even for finite-time interactions. Second, all four vacua have different capacities for creating correlations between the detectors, with the Vaidya vacuum interpolating between the Unruh vacuum near the horizon and the Boulware vacuum far from the horizon. Third, we show that the black hole horizon inhibits any correlations, not just entanglement. Finally, we show that the efficiency of the harvesting protocol depend strongly on the signalling ability of the detectors, which is highly non-trivial in presence of curvature. We provide an asymptotic analysis of the Vaidya vacuum to clarify the relationship between the Boulware/Unruh interpolation and the near/far from horizon and early/late-time limits. We demonstrate a straightforward implementation of numerical contour integration to perform all the calculations.

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Section: Resultsmentioning

confidence: 95%

“…The most formidable calculations of the two-point functions of this kind are done e.g. in [53,54], though the objectives are different.…”

Section: Jhep08(2020)155mentioning

confidence: 99%

Section: Jhep08(2020)155mentioning

confidence: 99%

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Harvesting correlations in Schwarzschild and collapsing shell spacetimes

Tjoa

Mann

2020

J. High Energ. Phys.

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“…To conclude, we arrived at the finding that, instead of using rods and clocks to map the curvature of a spacetime manifold, as Einstein envisaged, we could map the curvature of a spacetime manifold by measuring G F (x, x ′ ) close to its diagonal, i.e., by measuring the local correlations of quantum field fluctuations. This is because the Feynman propagator G F (x, x ′ ) can then be used to recover the traditional metric-based description of a spacetime through Equation (7). Intuitively, this is possible because the strength of the correlations of the quantum field fluctuations that is encoded in the propagator is a proxy for the covariant distance, the correlations being the stronger the smaller the covariant distance.…”

Section: Measuring Spacetime Distances By Means Of Correlatorsmentioning

confidence: 99%

“…This tells us that knowing the wave operator in its eigenbasis (i.e., knowing nothing but its spectrum) and, in addition, also knowing a unitary transformation from that eigenbasis to a position basis is sufficient to calculate the metric. This is because we can then transform the Feynman propagator or wave operator from the eigenbasis of the wave operator into a position basis and, from there, arrive at the metric using Equation (7).…”

Section: Identifying the Geometric Degrees Of Freedommentioning

confidence: 99%

Replacing the Notion of Spacetime Distance by the Notion of Correlation

Kempf

2021

Front. Phys.

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Spacetime is conventionally viewed as a stage on which actors, in the form of massive and massless matter, move. In this study, we explore what may lie beyond this picture. The starting point is the observation that quantum field fluctuations are the more strongly correlated the shorter their spacetime distance. The notion of spacetime distance can, therefore, be replaced by the notion of correlation strength. This suggests a new picture in which the abstract 2-point and multi-point correlations are the primary structure, a picture which is essentially information-theoretic. In the low energy regime, the secondary notions of spacetime and of matter would then emerge as approximate representations of the abstract correlators, namely, in the form of Feynman rules on curved spacetime.

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Qubits on the horizon: decoherence and thermalization near black holes

Kaplanek

Burgess

2021

J. High Energ. Phys.

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We examine the late-time evolution of a qubit (or Unruh-De Witt detector) that hovers very near to the event horizon of a Schwarzschild black hole, while interacting with a free quantum scalar field. The calculation is carried out perturbatively in the dimensionless qubit/field coupling g, but rather than computing the qubit excitation rate due to field interactions (as is often done), we instead use Open EFT techniques to compute the late-time evolution to all orders in g2t/rs (while neglecting order g4t/rs effects) where rs = 2GM is the Schwarzschild radius. We show that for qubits sufficiently close to the horizon the late-time evolution takes a simple universal form that depends only on the near-horizon geometry, assuming only that the quantum field is prepared in a Hadamard-type state (such as the Hartle-Hawking or Unruh vacua). When the redshifted energy difference, ω∞, between the two qubit states (as measured by a distant observer looking at the detector) satisfies ω∞rs ≪ 1 this universal evolution becomes Markovian and describes an exponential approach to equilibrium with the Hawking radiation, with the off-diagonal and diagonal components of the qubit density matrix relaxing to equilibrium with different characteristic times, both of order rs/g2.

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Communication through quantum fields near a black hole

Cited by 38 publications

References 63 publications

Harvesting correlations in Schwarzschild and collapsing shell spacetimes

Harvesting correlations in Schwarzschild and collapsing shell spacetimes

Replacing the Notion of Spacetime Distance by the Notion of Correlation

Qubits on the horizon: decoherence and thermalization near black holes

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