Quantum vacuum near non-rotating compact objects

Emelyanov, Viacheslav A.

doi:10.1088/1361-6382/aacb8b

Cited by 7 publications

(15 citation statements)

References 25 publications

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“…It is, probably, of interest to consider the limit

L \to 0

. This case corresponds to the local Minkowski vacuum, in which astrophysical black holes do not evaporate . Having set

L = 0

in (31), we find that the trace anomaly gives

ψ = 0

and

\begin{matrix} true \\ right ϕ & = & left - \frac{r_{H}^{2}}{180 π r^{3}}, \end{matrix}

that slightly reduces the event‐horizon size and is small at

r = r_{H}

even for a Planckian‐size black hole.…”

Section: Black‐hole Evaporationmentioning

confidence: 97%

“…At quantum level, however, the trace of T μ ν (x) is no longer trivial. In fact, any quan-tum state, which locally looks as the Minkowski vacuum, is described by a Feynman propagator which has the same singular part in the x → x limit as G M (x, x ) in (6). This, in turn, possesses a geometrical term which gives the trace anomaly after the renormalization (see, e.g., [5] for more details).…”

Section: Black-hole Evaporationmentioning

confidence: 99%

“…This case corresponds to the local Minkowski vacuum, in which astrophysical black holes do not evaporate. [6] Having set L = 0 in (31), we find that the trace anomaly gives ψ = 0 and www.advancedsciencenews.com www.fp-journal.org…”

Section: Black-hole Evaporationmentioning

confidence: 99%

“…6.2 in [3]). The first term on the right-hand side of (6) is the standard Feynman propagator for a massless scalar field used (as a toy model) in particle physics, in which the l c → ∞ limit is tacitly considered and, therefore, all curvature terms in (6) vanish. This explains our usage of the index in G M (x, x ), that stands for Minkowski.…”

Section: Introductionmentioning

confidence: 99%

“…This explains our usage of the index in G M (x, x ), that stands for Minkowski. [6] The local procedure towards field quantisation allows us to describe many-particle systems, which usually possess a finite space-time extent. For instance, if there is black-body radiation (R) due to the scalar field φ(x) inside a box (B) of the size l B l c , then this scalar-field radiation can be mathematically represented by…”

Section: Introductionmentioning

confidence: 99%

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Black‐Hole Evolution from Stellar Collapse

Emelyanov

2019

Fortschritte der Physik

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We present a local approach towards black‐hole evaporation, which relies on the absence of quantum phase transition across the stellar surface. We show that this approach augmented with Bekenstein's black‐hole entropy gives the Hawking effect if the null energy condition is violated in the initial quantum‐field vacuum. If otherwise, an astrophysical black hole may then be expanding, that corresponds to the anti‐Hawking effect, i.e. a positive‐energy radiation flows into the black hole, taking its origin far away from the event horizon. This quantum process is reverse to the Hawking effect, as the latter is described by a negative‐energy influx nearby the horizon, which goes over to a positive‐energy outflux in the far‐horizon region. We also provide examples of quantum vacua well‐known in the literature, which give rise to both quantum effects from stellar collapse.

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“…It is, probably, of interest to consider the limit

L \to 0

. This case corresponds to the local Minkowski vacuum, in which astrophysical black holes do not evaporate . Having set

L = 0

in (31), we find that the trace anomaly gives

ψ = 0

and

\begin{matrix} true \\ right ϕ & = & left - \frac{r_{H}^{2}}{180 π r^{3}}, \end{matrix}

that slightly reduces the event‐horizon size and is small at

r = r_{H}

even for a Planckian‐size black hole.…”

Section: Black‐hole Evaporationmentioning

confidence: 97%

Section: Black-hole Evaporationmentioning

confidence: 99%

Section: Black-hole Evaporationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Black‐Hole Evolution from Stellar Collapse

Emelyanov

2019

Fortschritte der Physik

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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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Qubit heating near a hotspot

Kaplanek

Burgess

Holman³

2021

J. High Energ. Phys.

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Effective theories describing black hole exteriors contain many open-system features due to the large number of gapless degrees of freedom that lie beyond reach across the horizon. A simple solvable Caldeira-Leggett type model of a quantum field interacting within a small area with many unmeasured thermal degrees of freedom was recently proposed in ref. [23] to provide a toy model of this kind of dynamics against which more complete black hole calculations might be compared. We here compute the response of a simple Unruh-DeWitt detector (or qubit) interacting with a massless quantum field ϕ coupled to such a hotspot. Our treatment differs from traditional treatments of Unruh-DeWitt detectors by using Open-EFT tools to reliably calculate the qubit’s late-time behaviour. We use these tools to determine the efficiency with which the qubit thermalizes as a function of its proximity to the hotspot. We identify a Markovian regime in which thermalization does occur, though only for qubits closer to the hotspot than a characteristic distance scale set by the ϕ-hotspot coupling. We compute the thermalization time, and find that it varies inversely with the ϕ-qubit coupling strength in the standard way.

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Quantum vacuum near non-rotating compact objects

Cited by 7 publications

References 25 publications

Black‐Hole Evolution from Stellar Collapse

Black‐Hole Evolution from Stellar Collapse

Qubits on the horizon: decoherence and thermalization near black holes

Qubit heating near a hotspot

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