CGHS Black Hole Analog Moving Mirror and Its Relativistic Quantum Information as Radiation Reaction

The Callan–Giddings–Harvey–Strominger black hole has a spectrum and temperature that correspond to an accelerated reflecting boundary condition in flat spacetime. The beta coefficients are identical to a moving mirror model, where the acceleration is exponential in laboratory time. The center of the black hole is modeled by the perfectly reflecting regularity condition that red-shifts the field modes, which is the source of the particle creation. In addition to computing the energy flux, we find the corresponding moving mirror parameter associated with the black hole mass and the cosmological constant in the gravitational analog system. Generalized to any mirror trajectory, we derive the self-force (Lorentz–Abraham–Dirac), consistently, expressing it and the Larmor power in connection with entanglement entropy, inviting an interpretation of acceleration radiation in terms of information flow. The mirror self-force and radiative power are applied to the particular CGHS black hole analog moving mirror, which reveals the physics of information at the horizon during asymptotic approach to thermal equilibrium.

Download Full-text

Light and Airy: A Simple Solution for Relativistic Quantum Acceleration Radiation

Universe ◽

10.3390/universe7030060 ◽

2021 ◽

Vol 7 (3) ◽

pp. 60

Author(s):

Michael R. R. Good ◽

Eric V. Linder

Keyword(s):

Particle Production ◽

Casimir Effect ◽

Relativistic Quantum ◽

Entanglement Entropy ◽

Particle Creation ◽

Finite Energy ◽

Negative Energy ◽

Dynamical Casimir Effect ◽

Quantum Radiation ◽

General Relations

We study the quantum radiation of particle production by vacuum from an ultra-relativistic moving mirror (dynamical Casimir effect) solution that allows (possibly for the first time) analytically calculable time evolution of particle creation and an Airy particle spectral distribution. The reality of the beta Bogoliubov coefficients is responsible for the simplicity, and the mirror is asymptotically inertial at the speed of light, with finite energy production. We also discuss general relations regarding negative energy flux, the transformation to the 1-D Schrödinger equation, and the incompleteness of entanglement entropy.

Download Full-text

Horizon radiation reaction forces

Journal of High Energy Physics ◽

10.1007/jhep10(2020)026 ◽

2020 ◽

Vol 2020 (10) ◽

Author(s):

Walter D. Goldberger ◽

Ira Z. Rothstein

Keyword(s):

Black Hole ◽

Equations Of Motion ◽

Finite Size ◽

Radiation Reaction ◽

Effective Field ◽

Compact Objects ◽

Finite Size Effect ◽

Binary Black Holes ◽

Dissipative Effects ◽

Reaction Forces

Abstract Using Effective Field Theory (EFT) methods, we compute the effects of horizon dissipation on the gravitational interactions of relativistic binary black hole systems. We assume that the dynamics is perturbative, i.e it admits an expansion in powers of Newton’s constant (post-Minkowskian, or PM, approximation). As applications, we compute corrections to the scattering angle in a black hole collision due to dissipative effects to leading PM order, as well as the post-Newtonian (PN) corrections to the equations of motion of binary black holes in non-relativistic orbits, which represents the leading order finite size effect in the equations of motion. The methods developed here are also applicable to the case of more general compact objects, eg. neutron stars, where the magnitude of the dissipative effects depends on non-gravitational physics (e.g, the equation of state for nuclear matter).

Download Full-text

Islands and stretched horizon

Journal of High Energy Physics ◽

10.1007/jhep07(2021)051 ◽

2021 ◽

Vol 2021 (7) ◽

Author(s):

Yoshinori Matsuo

Keyword(s):

Black Holes ◽

Black Hole ◽

Hawking Radiation ◽

Entanglement Entropy ◽

Total System ◽

Island Rule ◽

Asymptotically Flat ◽

Flat Spacetime ◽

Ads Spacetime ◽

Hole Geometry

Abstract Recently it was proposed that the entanglement entropy of the Hawking radiation contains the information of a region including the interior of the event horizon, which is called “island.” In studies of the entanglement entropy of the Hawking radiation, the total system in the black hole geometry is separated into the Hawking radiation and black hole. In this paper, we study the entanglement entropy of the black hole in the asymptotically flat Schwarzschild spacetime. Consistency with the island rule for the Hawking radiation implies that the information of the black hole is located in a different region than the island. We found an instability of the island in the calculation of the entanglement entropy of the region outside a surface near the horizon. This implies that the region contains all the information of the total system and the information of the black hole is localized on the surface. Thus the surface would be interpreted as the stretched horizon. This structure also resembles black holes in the AdS spacetime with an auxiliary flat spacetime, where the information of the black hole is localized at the interface between the AdS spacetime and the flat spacetime.

Download Full-text

First law of entanglement entropy in AdS black hole backgrounds

Physical Review D ◽

10.1103/physrevd.104.026004 ◽

2021 ◽

Vol 104 (2) ◽

Author(s):

Akihiro Ishibashi ◽

Kengo Maeda

Keyword(s):

Black Hole ◽

Entanglement Entropy

Download Full-text

Islands in linear dilaton black holes

Journal of High Energy Physics ◽

10.1007/jhep03(2021)253 ◽

2021 ◽

Vol 2021 (3) ◽

Cited By ~ 1

Author(s):

Georgios K. Karananas ◽

Alex Kehagias ◽

John Taskas

Keyword(s):

Black Holes ◽

Black Hole ◽

Entanglement Entropy ◽

Von Neumann Entropy ◽

Two Dimensional ◽

Extremal Case ◽

Von Neumann ◽

Dimensional Black Hole ◽

Linear Dilaton ◽

Linear Dilaton Black Hole

Abstract We derive a novel four-dimensional black hole with planar horizon that asymptotes to the linear dilaton background. The usual growth of its entanglement entropy before Page’s time is established. After that, emergent islands modify to a large extent the entropy, which becomes finite and is saturated by its Bekenstein-Hawking value in accordance with the finiteness of the von Neumann entropy of eternal black holes. We demonstrate that viewed from the string frame, our solution is the two-dimensional Witten black hole with two additional free bosons. We generalize our findings by considering a general class of linear dilaton black hole solutions at a generic point along the σ-model renormalization group (RG) equations. For those, we observe that the entanglement entropy is “running” i.e. it is changing along the RG flow with respect to the two-dimensional worldsheet length scale. At any fixed moment before Page’s time the aforementioned entropy increases towards the infrared (IR) domain, whereas the presence of islands leads the running entropy to decrease towards the IR at later times. Finally, we present a four-dimensional charged black hole that asymptotes to the linear dilaton background as well. We compute the associated entanglement entropy for the extremal case and we find that an island is needed in order for it to follow the Page curve.

Download Full-text

Self-force on a charge outside a five-dimensional black hole

Physical Review D ◽

10.1103/physrevd.89.124014 ◽

2014 ◽

Vol 89 (12) ◽

Cited By ~ 14

Author(s):

Matthew J. S. Beach ◽

Eric Poisson ◽

Bernhard G. Nickel

Keyword(s):

Black Hole ◽

Dimensional Black Hole ◽

A Charge ◽

Self Force

Download Full-text

Islands and Page curves of Reissner-Nordström black holes

Journal of High Energy Physics ◽

10.1007/jhep04(2021)103 ◽

2021 ◽

Vol 2021 (4) ◽

Author(s):

Xuanhua Wang ◽

Ran Li ◽

Jin Wang

Keyword(s):

Black Holes ◽

Black Hole ◽

Hawking Radiation ◽

Entanglement Entropy ◽

Additional Term ◽

Current Case ◽

Information Paradox ◽

Extremal Surface ◽

Four Dimensions ◽

Black Hole Information

Abstract We apply the recently proposed quantum extremal surface construction to calculate the Page curve of the eternal Reissner-Nordström black holes in four dimensions ignoring the backreaction and the greybody factor. Without the island, the entropy of Hawking radiation grows linearly with time, which results in the information paradox for the eternal black holes. By extremizing the generalized entropy that allows the contributions from the island, we find that the island extends to the outside the horizon of the Reissner-Nordström black hole. When taking the effect of the islands into account, it is shown that the entanglement entropy of Hawking radiation at late times for a given region far from the black hole horizon reproduces the Bekenstein-Hawking entropy of the Reissner-Nordström black hole with an additional term representing the effect of the matter fields. The result is consistent with the finiteness of the entanglement entropy for the radiation from an eternal black hole. This facilitates to address the black hole information paradox issue in the current case under the above-mentioned approximations.

Download Full-text