Black-hole Information Loss Problem: Past, Present, and Future

2020 ◽  
Vol 29 (11) ◽  
pp. 17-25
Author(s):  
Sang-Heon YI ◽  
Dong-han YEOM
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Mechanics ◽  
Quantum Information ◽  
Hawking Radiation ◽  
Recent Progress ◽  
Information Loss ◽  
Future Perspectives ◽  
Black Hole Information ◽  
Information Loss Problem

In this article, we discuss the information loss problem of black holes and critically review candidate resolutions of the problem. As a black hole evaporates via Hawking radiation, it seems to lose original quantum information; this indicates that the unitarity of time evolution in quantum mechanics and the fundamental predictability of physics are lost. We categorized candidate resolutions by asking (1) where information is and (2) which principle of physics is changed. We also briefly comment on the recent progress in the string theory community. Finally, we present several remarks for future perspectives.

scholarly journals Gravitational Waves Carry Information about the Infalling Matter out of Black Holes: a Resolution of the Black Hole Information Paradox

2020 ◽  
Author(s):  
Xueyi Tian
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Black Hole ◽  
Quantum Mechanics ◽  
Gravitational Waves ◽  
Hawking Radiation ◽  
Information Loss ◽  
Information Paradox ◽  
Black Hole Information ◽  
The Universe

The black hole information paradox is one of the most puzzling paradoxes in physics. Black holes trap everything that falls into them, while their mass may leak away through purely thermal Hawking radiation. When a black hole vanishes, all the information locked inside, if any, is just lost, thus challenging the principles of quantum mechanics. However, some information does have a way to escape from inside the black hole, that is, through gravitational waves. Here, a concise extension of this notion is introduced. When a black hole swallows something, whether it is a smaller black hole or an atom, the system emits gravitational waves carrying the information about the “food”. Although most of the signals are too weak to be detected, the information encoded within them will persist in the universe. This speculation provides an explanation for a large part, if not all, of the supposed “information loss” in black holes, and thus reconciles the predictions of general relativity and quantum mechanics.

Thermodynamics, Quantum Physics, and Black Holes

2020 ◽  
pp. 24-39
Author(s):  
John W. Moffat
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Mechanics ◽  
Quantum Physics ◽  
Second Law Of Thermodynamics ◽  
Information Loss ◽  
Second Law ◽  
Major Question ◽  
Long Time ◽  
Information Loss Problem

A major question confronting physicists studying black holes was whether thermodynamics applied to them—that is, whether the black holes radiated heat and lost energy. Bekenstein considered heat and thermodynamics important for the interior of black holes. Based on the second law of thermodynamics, Hawking proposed that black holes evaporate over a very long time through what we now call Hawking radiation. This concept contradicts the notion that nothing can escape a black hole event horizon. Quantum physics enters into Hawking’s calculations, and he discovered the conundrum that the radiation would violate quantum mechanics, leading to what is called the information loss problem. These ideas are still controversial, and many physicists have attempted to resolve them, including Russian theorists Zel’dovich and Starobinsky. Alternative quantum physics interpretations of black holes have been proposed that address the thermodynamics problems, including so-called gravastars.

scholarly journals Information recovery from evaporating black holes

2021 ◽  
pp. 2150069
Author(s):  
Samuel L. Braunstein ◽  
Saurya Das ◽  
Zhi-Wei Wang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Information ◽  
Apparent Horizon ◽  
Information Loss ◽  
Information Recovery ◽  
Rotating Black Hole ◽  
Information Loss Problem

We show that the apparent horizon and the region near [Formula: see text] of an evaporating charged, rotating black hole are timelike. It then follows that black holes in nature, which invariably have some rotation, have a channel, via which classical or quantum information can escape to the outside, while the black hole shrinks in size. We discuss implications for the information loss problem.

scholarly journals Islands and Page curves of Reissner-Nordström black holes

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.

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

2020 ◽  
Vol 2020 (4) ◽  
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.

scholarly journals Corrected Hawking Radiation of Dirac Particles from a General Static Riemann Black Hole

2013 ◽  
Vol 2013 ◽  
pp. 1-6 ◽  
Author(s):  
Ge-Rui Chen ◽  
Yong-Chang Huang
Keyword(s):  
Black Hole ◽  
Quantum Theory ◽  
Hawking Radiation ◽  
Radiation Spectrum ◽  
Direct Consequence ◽  
Information Loss ◽  
Back Reaction ◽  
Information Loss Paradox ◽  
Dirac Particles ◽  
Black Hole Information

Considering energy conservation and the back reaction of radiating particles to the spacetime, we investigate the massive Dirac particles' Hawking radiation from a general static Riemann black hole using improved Damour-Ruffini method. A direct consequence is that the radiation spectrum is not strictly thermal. The correction to the thermal spectrum is consistent with an underlying unitary quantum theory and this may have profound implications for the black hole information loss paradox.

scholarly journals INFORMATION CONSERVATION IS FUNDAMENTAL: RECOVERING THE LOST INFORMATION IN HAWKING RADIATION

2013 ◽  
Vol 22 (12) ◽  
pp. 1341014 ◽  
Author(s):  
BAOCHENG ZHANG ◽  
QING-YU CAI ◽  
MING-SHENG ZHAN ◽  
LI YOU
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Energy Charge ◽  
Fundamental Principle ◽  
Information Loss ◽  
Information Loss Paradox ◽  
Information Conservation ◽  
World Information ◽  
Conservation Laws Of Energy

In both classical and quantum world, information cannot appear or disappear. This fundamental principle, however, is questioned for a black hole, by the acclaimed "information loss paradox." Based on the conservation laws of energy, charge, and angular momentum, we recently show the total information encoded in the correlations among Hawking radiations equals exactly to the same amount previously considered lost, assuming the nonthermal spectrum of Parikh and Wilczek. Thus the information loss paradox can be falsified through experiments by detecting correlations, for instance, through measuring the covariances of Hawking radiations from black holes, such as the manmade ones speculated to appear in LHC experiments. The affirmation of information conservation in Hawking radiation will shine new light on the unification of gravity with quantum mechanics.

Thermal relativity, modified Hawking radiation, and the generalized uncertainty principle

2019 ◽  
Vol 16 (10) ◽  
pp. 1950156
Author(s):  
Carlos Castro Perelman
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Uncertainty Relation ◽  
Generalized Uncertainty Principle ◽  
Black Hole Entropy ◽  
The Novel ◽  
Black Hole Information ◽  
The One ◽  
Mini Black Holes

After a brief review of the thermal relativistic corrections to the Schwarzschild black hole entropy, it is shown how the Stefan–Boltzman law furnishes large modifications to the evaporation times of Planck-size mini-black holes, and which might furnish important clues to the nature of dark matter and dark energy since one of the novel consequences of thermal relativity is that black holes do not completely evaporate but leave a Planck size remnant. Equating the expression for the modified entropy (due to thermal relativity corrections) with Wald’s entropy should, in principle, determine the functional form of the modified gravitational Lagrangian [Formula: see text]. We proceed to derive the generalized uncertainty relation which corresponds to the effective temperature [Formula: see text] associated with thermal relativity and given in terms of the Hawking ([Formula: see text]) and Planck ([Formula: see text]) temperature, respectively. Such modified uncertainty relation agrees with the one provided by string theory up to first order in the expansion in powers of [Formula: see text]. Both lead to a minimal length (Planck size) uncertainty. Finally, an explicit analytical expression is found for the modifications to the purely thermal spectrum of Hawking radiation which could cast some light into the resolution of the black hole information paradox.

scholarly journals Quantum Hair on Colliding Black Holes

Entropy ◽  
2020 ◽  
Vol 22 (3) ◽  
pp. 301
Author(s):  
Lawrence Crowell ◽  
Christian Corda
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Mechanics ◽  
Quantum Information ◽  
Excited States ◽  
Gravitational Radiation ◽  
Quantum Physics ◽  
Quantum Limit ◽  
Event Horizons ◽  
Quasi Normal Mode

Black hole (BH) collisions produce gravitational radiation which is generally thought, in a quantum limit, to be gravitons. The stretched horizon of a black hole contains quantum information, or a form of quantum hair, which is a coalescence of black holes participating in the generation of gravitons. This may be facilitated with a Bohr-like approach to black hole (BH) quantum physics with quasi-normal mode (QNM) approach to BH quantum mechanics. Quantum gravity and quantum hair on event horizons is excited to higher energy in BH coalescence. The near horizon condition for two BHs right before collision is a deformed A d S spacetime. These excited states of BH quantum hair then relax with the production of gravitons. This is then argued to define RT entropy given by quantum hair on the horizons. These qubits of information from a BH coalescence should then appear in gravitational wave (GW) data.

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