Quantum simulation of black-hole radiation

The holographic principle has taught us that, as far as their entropy content is concerned, black holes in (3 + 1)-dimensional curved spacetimes behave as ordinary thermodynamic systems in flat (2 + 1)-dimensional spacetimes. In this paper, we point out that the opposite behavior can also be observed in black-hole physics. To show this we study the quantum Hawking evaporation of near-extremal Reissner–Nordström (RN) black holes. We first point out that the black-hole radiation spectrum departs from the familiar radiation spectrum of genuine (3 + 1)-dimensional perfect black-body emitters. In particular, the would be black-body thermal spectrum is distorted by the curvature potential which surrounds the black-hole and effectively blocks the emission of low-energy quanta. Taking into account the energy-dependent gray-body factors which quantify the imprint of passage of the emitted radiation quanta through the black-hole curvature potential, we reveal that the (3 + 1)-dimensional black holes effectively behave as perfect black-body emitters in a flat (9 + 1)-dimensional spacetime.

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Spectral properties of acoustic black hole radiation: Broadening the horizon

Physical Review D ◽

10.1103/physrevd.83.084010 ◽

2011 ◽

Vol 83 (8) ◽

Cited By ~ 32

Author(s):

Stefano Finazzi ◽

Renaud Parentani

Keyword(s):

Black Hole ◽

Spectral Properties ◽

Black Hole Radiation

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More on extracting information about the initial state from the black hole radiation

Modern Physics Letters A ◽

10.1142/s0217732318501080 ◽

2018 ◽

Vol 33 (19) ◽

pp. 1850108

Author(s):

Hossein Ghaforyan ◽

Somayyeh Shoorvazi ◽

Alireza Sepehri ◽

Tooraj Ghaffary

Keyword(s):

Black Holes ◽

Black Hole ◽

Density Matrix ◽

Quantum Entanglement ◽

Event Horizon ◽

Initial State ◽

Black Hole Radiation ◽

Total Information ◽

Quantum Treatment ◽

Collapse Process

Recently, some authors showed that a classical collapse scenario ignores this richness of information in the resulting spectrum and a consistent quantum treatment of the entire collapse process might allow us to retrieve much more information from the spectrum of the final radiation. We confirm these results and show that by considering the quantum entanglement between metrics, we can uncover information of black holes. In our model, a density matrix is defined for the spaces, both inside and outside of the event horizon. These inside and outside spaces of black holes are obtained by tracing from a bigger space. An observer that lives in this big space can recover total information regarding the inside and outside of black hole.

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Phase connected X-ray light curve and He II radial velocity measurements of NGC 300 X-1

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318007615 ◽

2018 ◽

Vol 14 (S346) ◽

pp. 187-192

Author(s):

S. Carpano ◽

F. Haberl ◽

P. Crowther ◽

A. Pollock

Keyword(s):

Black Hole ◽

Light Curve ◽

Radial Velocity ◽

Orbital Period ◽

High Mass ◽

Velocity Measurements ◽

X Ray ◽

Black Hole Radiation ◽

Ic 10 ◽

Binary Evolution

Abstract. NGC 300 X-1 and IC 10 X-1 are currently the only two robust extragalactic candidates for being Wolf-Rayet/black hole X-ray binaries, the Galactic analogue being Cyg X-3. These systems are believed to be a late product of high-mass X-ray binary evolution and direct progenitors of black hole mergers. From the analysis of Swift data, the orbital period of NGC 300 X-1 was found to be 32.8 h. We here merge the full set of existing data of NGC 300 X-1, using XMM-Newton, Chandra and Swift observations to derive a more precise value of the orbital period of 32.7932 ± 0.0029 h above a confidence level of 99.99%. This allows us to phase connect the X-ray light curve of the source with radial velocity measurements of He II lines performed in 2010. We show that, as for IC 10 X-1 and Cyg X-3, the X-ray eclipse corresponds to maximum of the blueshift of the He II lines, instead of the expected zero velocity. This indicates that for NGC 300 X-1 as well, the wind of the WR star is completely ionised by the black hole radiation and that the emission lines come from the region of the WR star that is in the shadow. We also present for the first time the light curve of two recent very long XMM-Newton observations of the source, performed on the 16th to 20th of December 2016.

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A quantum-corrected approach to black hole radiation via a tunneling process

Progress of Theoretical and Experimental Physics ◽

10.1093/ptep/ptaa032 ◽

2020 ◽

Vol 2020 (4) ◽

Cited By ~ 2

Author(s):

Milad Hajebrahimi ◽

Kourosh Nozari

Keyword(s):

Black Hole ◽

Electric Charge ◽

Hawking Radiation ◽

Quantum Correction ◽

Black Hole Physics ◽

Information Loss ◽

Schwarzschild Black Hole ◽

Tunneling Process ◽

Black Hole Radiation ◽

Information Loss Problem

Abstract In the language of black hole physics, Hawking radiation is one of the most controversial subjects about which there exist lots of puzzles, including the information loss problem and the question of whether this radiation is thermal or not. In this situation, a possible way to face these problems is to bring quantum effects into play, also taking into account self-gravitational effects in the scenario. We consider a quantum-corrected form of the Schwarzschild black hole inspired by the pioneering work of Kazakov and Solodukhin to modify the famous Parikh–Wilczek tunneling process for Hawking radiation. We prove that in this framework the radiation is not thermal, with a correlation function more effective than the Parikh–Wilczek result, and the information loss problem can be addressed more successfully. Also, we realize that quantum correction affects things in the same way as an electric charge. So, it seems that quantum correction in this framework has something to do with the electric charge.

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