The black hole information paradox[1] is a puzzle resulting from the combination of quantum mechanics and general relativity. Calculations suggest that physical information could permanently disappear in a black hole, allowing many physical states to devolve into the same state. This is controversial because it violates a core precept of modern physics—that in principle the value of a wave function of a physical system at one point in time should determine its value at any other time.[2][3] A fundamental postulate of the Copenhagen interpretation of quantum mechanics is that complete information about a system is encoded in its wave function up to when the wave function collapses. The evolution of the wave function is determined by a unitary operator, and unitarity implies that information is conserved in the quantum sense.

As of November 2019, the paradox may have been resolved, at least for simplified models of gravity (see § Recent developments).

Relevant principles

There are two main principles in play:[4]

Quantum determinism means that given a present wave function, its future changes are uniquely determined by the evolution operator.

Reversibility refers to the fact that the evolution operator has an inverse, meaning that the past wave functions are similarly unique.

The combination of the two means that information must always be preserved.

Starting in the mid-1970s, Stephen Hawking and Jacob Bekenstein put forward theoretical arguments based on general relativity and quantum field theory that not only appeared to be inconsistent with information conservation but which did not account for the information loss and which stated no reason for it. Specifically, Hawking's calculations[5] indicated that black hole evaporation via Hawking radiation does not preserve information. Today, many physicists believe that the holographic principle (specifically the AdS/CFT duality) demonstrates that Hawking's conclusion was incorrect, and that information is in fact preserved.[6] In 2004 Hawking himself conceded a bet he had made, agreeing that black hole evaporation does in fact preserve information.

Hawking radiation

Main article: Hawking radiation

The Penrose diagram of a black hole which forms, and then completely evaporates away. Time shown on vertical axis from bottom to top; space shown on horizontal axis from left (radius zero) to right (growing radius).

In 1973–75, Stephen Hawking and Jacob Bekenstein showed that black holes should slowly radiate away energy, which poses a problem. From the no-hair theorem, one would expect the Hawking radiation to be completely independent of the material entering the black hole. Nevertheless, if the material entering the black hole were a pure quantum state, the transformation of that state into the mixed state of Hawking radiation would destroy information about the original quantum state. This violates Liouville's theorem and presents a physical paradox.

Hawking remained convinced that the equations of black-hole thermodynamics, together with the no-hair theorem, led to the conclusion that quantum information may be destroyed. This annoyed many physicists, notably John Preskill, who in 1997 bet Hawking and Kip Thorne that information was not lost in black holes. The implications that Hawking had opened led to a "battle" where Leonard Susskind and Gerard 't Hooft publicly 'declared war' on Hawking's solution, with Susskind publishing a popular book, The Black Hole War, about the debate in 2008. (The book carefully notes that the 'war' was purely a scientific one, and that at a personal level, the participants remained friends.[7]) The solution to the problem that concluded the battle is the holographic principle, which was first proposed by 't Hooft but was given a precise string theory interpretation by Susskind. With this, "Susskind quashes Hawking in quarrel over quantum quandary".[8]

There are various ideas about how the paradox is solved. Since the 1997 proposal of the AdS/CFT correspondence, the predominant belief among physicists is that information is preserved and that Hawking radiation is not precisely thermal but receives quantum corrections that encode information about the black hole's interior. This viewpoint received further support in 2019 when researchers amended the computation of the entropy of the Hawking radiation in certain models, and showed that the radiation is in fact dual to the black hole interior at late times.[9][10] Other possibilities include the information being contained in a Planckian remnant left over at the end of Hawking radiation or a modification of the laws of quantum mechanics to allow for non-unitary time evolution.

In July 2004, Stephen Hawking published a paper presenting a theory that quantum perturbations of the event horizon could allow information to escape from a black hole, which would resolve the information paradox.[11] His argument assumes the unitarity of the AdS/CFT correspondence which implies that an AdS black hole that is dual to a thermal conformal field theory. When announcing his result, Hawking also conceded the 1997 bet, paying Preskill with a baseball encyclopedia "from which information can be retrieved at will."

According to Roger Penrose, loss of unitarity in quantum systems is not a problem: quantum measurements are by themselves already non-unitary. Penrose claims that quantum systems will in fact no longer evolve unitarily as soon as gravitation comes into play, precisely as in black holes. The Conformal Cyclic Cosmology advocated by Penrose critically depends on the condition that information is in fact lost in black holes. This new cosmological model might in the future be tested experimentally by detailed analysis of the cosmic microwave background radiation (CMB): if true, the CMB should exhibit circular patterns with slightly lower or slightly higher temperatures. In November 2010, Penrose and V. G. Gurzadyan announced they had found evidence of such circular patterns, in data from the Wilkinson Microwave Anisotropy Probe (WMAP) corroborated by data from the BOOMERanG experiment.[12] The significance of the findings was subsequently debated by others.[13][14][15][16]

Postulated solutions

Information is irretrievably lost[17][18]

Advantage: Seems to be a direct consequence of relatively non-controversial calculation based on semiclassical gravity.

Disadvantage: Violates unitarity. (Banks, Susskind and Peskin argued that it also violates energy-momentum conservation or locality, but the argument does not seem to be correct for systems with a large number of degrees of freedom.[19])

Information gradually leaks out during the black-hole evaporation[17][18]

Advantage: Intuitively appealing because it qualitatively resembles information recovery in a classical process of burning.

Disadvantage: Requires a large deviation from classical and semiclassical gravity (which do not allow information to leak out from the black hole) even for macroscopic black holes for which classical and semiclassical approximations are expected to be good approximations.

Information suddenly escapes out during the final stage of black-hole evaporation[17][18]

Advantage: A significant deviation from classical and semiclassical gravity is needed only in the regime in which the effects of quantum gravity are expected to dominate.

Disadvantage: Just before the sudden escape of information, a very small black hole must be able to store an arbitrary amount of information, which violates the Bekenstein bound.

Information is stored in a Planck-sized remnant[17][18]

Advantage: No mechanism for information escape is needed.

Disadvantage: To contain the information from any evaporated black hole, the remnants would need to have an infinite number of internal states. It has been argued that it would be possible to produce an infinite amount of pairs of these remnants since they are small and indistinguishable from the perspective of the low-energy effective theory.[20]

Information is stored in a large remnant[21][22]

Advantage: The size of remnant increases with the size of the initial black hole, so there is no need for an infinite number of internal states.

Disadvantage: Hawking radiation must stop before the black hole reaches the Planck size, which requires a violation of semi-classical gravity at a macroscopic scale.

Information is stored in a baby universe that separates from our own universe.[18][23]

Advantage: This scenario is predicted by the Einstein–Cartan theory of gravity which extends general relativity to matter with intrinsic angular momentum (spin). No violation of known general principles of physics is needed.

Disadvantage: It is difficult to test the Einstein–Cartan theory because its predictions are significantly different from general-relativistic ones only at extremely high densities.

Information is encoded in the correlations between future and past[24][25]

Advantage: Semiclassical gravity is sufficient, i.e., the solution does not depend on details of (still not well understood) quantum gravity.

Disadvantage: Contradicts the intuitive view of nature as an entity that evolves with time.

Recent developments

In 2014, Chris Adami argued that analysis using quantum channel theory causes any apparent paradox to disappear; Adami rejects Susskind's analysis of black hole complementarity, arguing instead that no space-like surface contains duplicated quantum information.[26][27]

In 2015, Modak, Ortíz, Peña and Sudarsky, have argued that the paradox can be dissolved by invoking foundational issues of quantum theory often referred as the measurement problem of quantum mechanics.[28] This work was built on an earlier proposal by Okon and Sudarsky on the benefits of objective collapse theory in a much broader context.[29] The original motivation of these studies was the long lasting proposal of Roger Penrose where collapse of the wave-function is said to be inevitable in presence of black holes (and even under the influence of gravitational field).[30][31] Experimental verification of collapse theories is an ongoing effort.[32]

In 2016, Hawking et al. proposed new theories of information moving in and out of a black hole.[33][34] The 2016 work posits that the information is saved in "soft particles", low-energy versions of photons and other particles that exist in zero-energy empty space.[35]

Significant progress was made in 2019, when Penington et al. discovered a class of semiclassical spacetime geometries that had been overlooked by Hawking and subsequent researchers.[9][10][36] Hawking's calculation appears to show that the Hawking radiation's entropy increases throughout the lifetime of the black hole. However, if the black hole formed from a known state (zero entropy), the entropy of the Hawking radiation must decrease back to zero once the black hole evaporates completely. Penington et al. compute the entropy using the replica trick, and show that for sufficiently old black holes, one must consider solutions in which the replicas are connected by wormholes. The inclusion of these wormhole geometries prevents the entropy from increasing indefinitely.

This result appears to resolve the information paradox, at least in the simple gravity theories that they consider. Although the replicas do not have direct physical meaning, the appearance of wormholes carries over to a physical description of the system. In particular, for sufficiently old black holes, one can perform operations on the Hawking radiation that affect the black hole interior. This result has implications for the related firewall paradox, and resembles the proposed ER=EPR resolution.

See also

AdS/CFT correspondence

Beyond black holes

Black hole complementarity

Cosmic censorship hypothesis

Firewall (physics)

Fuzzball (string theory)

Holographic principle

List of paradoxes

Maxwell's Demon

No-hair theorem

Thorne–Hawking–Preskill bet

References

The short form "ínformation paradox" is also used for the Arrow information paradox.

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Black holes

Types

Schwarzschild Rotating Charged Virtual Kugelblitz Primordial Planck particle

Size

Micro

Extremal Electron Stellar

Microquasar Intermediate-mass Supermassive

Active galactic nucleus Quasar Blazar

Formation

Stellar evolution Gravitational collapse Neutron star

Related links Tolman–Oppenheimer–Volkoff limit White dwarf

Related links Supernova

Related links Hypernova Gamma-ray burst Binary black hole

Properties

Gravitational singularity

Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere

Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics

Immirzi parameter Schwarzschild radius Spaghettification

Issues

Black hole complementarity Information paradox Cosmic censorship ER=EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem

Metrics

Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward

Alternatives

Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball

Analogs

Optical black hole Sonic black hole

Lists

Black holes Most massive Nearest Quasars Microquasars

Related

Black Hole Initiative Black hole starship Compact star Exotic star

Quark star Preon star Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Quasi-star Rossi X-ray Timing Explorer Timeline of black hole physics White hole Wormhole

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