Black hole information paradox

Puzzle of disappearance of information in a black hole

The first image (silhouette or shadow) of a black hole, taken of the supermassive black hole in M87 with the Event Horizon Telescope, released in April 2019

The black hole information paradox[1] is a paradox that appears when the predictions of quantum mechanics and general relativity are combined. The theory of general relativity predicts the existence of black holes that are regions of spacetime from which nothing—not even light—can escape. In the 1970s, Stephen Hawking applied the semiclassical approach of quantum field theory in curved spacetime to such systems and found that an isolated black hole would emit a form of radiation (now called Hawking radiation in his honor). He also argued that the detailed form of the radiation would be independent of the initial state of the black hole,[2] and depend only on its mass, electric charge and angular momentum.

The information paradox appears when one considers a process in which a black hole is formed through a physical process and then evaporates away entirely through Hawking radiation. Hawking's calculation suggests that the final state of radiation would retain information only about the total mass, electric charge and angular momentum of the initial state. Since many different states can have the same mass, charge and angular momentum, this suggests that many initial physical states could evolve into the same final state. Therefore, information about the details of the initial state would be permanently lost; however, this violates a core precept of both classical and quantum physics: that, in principle only, the state of a system at one point in time should determine its state at any other time.[3][4] Specifically, in quantum mechanics the state of the system is encoded by its wave function. The evolution of the wave function is determined by a unitary operator, and unitarity implies that the wave function at any instant of time can be used to determine the wave function either in the past or the future. In 1993, Don Page argued that if a black hole starts in a pure quantum state and evaporates completely by a unitary process, the von Neumann entropy of the Hawking radiation initially increases and then decreases back to zero when the black hole has disappeared.[5] This is called the Page curve.[6]

It is now generally believed that information is preserved in black-hole evaporation.[7][8][9] For many researchers, deriving the Page curve is synonymous with solving the black hole information puzzle.[10]: 291 But views differ as to precisely how Hawking's original semiclassical calculation should be corrected.[8][9][11][12] In recent years, several extensions of the original paradox have been explored. Taken together, these puzzles about black hole evaporation have implications for how gravity and quantum mechanics must be combined. The information paradox remains an active field of research in quantum gravity.

## Relevant principles

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In quantum mechanics, the evolution of the state is governed by the Schrödinger equation. The Schrödinger equation obeys two principles that are relevant to the paradox—quantum determinism, which means that given a present wave function, its future changes are uniquely determined by the evolution operator, and reversibility, which 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.[13] In this context "information" means all the details of the state, and the statement that information must be preserved means that details corresponding to an earlier time can always be reconstructed at a later time.

Mathematically, the Schrödinger equation implies that the wavefunction at a time t1 can be related to the wavefunction at a time t2 by means of a unitary operator.  | Ψ ( t 1 ) ⟩ = U ( t 1 , t 2 ) | Ψ ( t 2 ) ⟩ . {\displaystyle |\Psi (t_{1})\rangle =U(t_{1},t_{2})|\Psi (t_{2})\rangle .} Since the unitary operator is bijective, the wavefunction at t2 can be obtained from the wavefunction at t1 and vice versa.

The reversibility of time evolution described above applies only at the microscopic level, since the wavefunction provides a complete description of the state. It should not be conflated with thermodynamic irreversibility. A process may appear irreversible if one keeps track only of the system's coarse-grained features and not of its microscopic details, as is usually done in thermodynamics. But at the microscopic level, the principles of quantum mechanics imply that every process is completely reversible.

Starting in the mid-1970s, Stephen Hawking and Jacob Bekenstein put forward theoretical arguments that suggested that black-hole evaporation loses information, and is therefore inconsistent with unitarity. Crucially, these arguments were meant to apply at the microscopic level and suggested that black-hole evaporation is not only thermodynamically but microscopically irreversible. This contradicts the principle of unitarity described above and leads to the information paradox. Since the paradox suggested that quantum mechanics would be violated by black-hole formation and evaporation, Hawking framed the paradox in terms of the "breakdown of predictability in gravitational collapse".[2]

The arguments for microscopic irreversibility were backed by Hawking's calculation of the spectrum of radiation that isolated black holes emit.[14] This calculation utilized the framework of general relativity and quantum field theory. The calculation of Hawking radiation is performed at the black hole horizon and does not account for the backreaction of spacetime geometry; for a large enough black hole the curvature at the horizon is small and therefore both these theories should be valid. Hawking relied on the no-hair theorem to arrive at the conclusion that radiation emitted by black holes would depend only on a few macroscopic parameters, such as the black hole's mass, charge, and spin, but not on the details of the initial state that led to the formation of the black hole. In addition, the argument for information loss relied on the causal structure of the black hole spacetime, which suggests that information in the interior should not affect any observation in the exterior, including observations performed on the radiation the black hole emits. If so, the region of spacetime outside the black hole would lose information about the state of the interior after black-hole evaporation, leading to the loss of information.

Today, some 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.[15] Moreover, recent analyses indicate that in semiclassical gravity the information loss paradox cannot be formulated in a self-consistent manner due to the impossibility of simultaneously realizing all of the necessary assumptions required for its formulation.[16][17]

## Black hole evaporation

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### Hawking radiation

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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 1973–1975, Stephen Hawking showed that black holes should slowly radiate away energy, and he later argued that this leads to a contradiction with unitarity. Hawking used the classical no-hair theorem to argue that the form of this radiation—called Hawking radiation—would be completely independent of the initial state of the star or matter that collapsed to form the black hole. He argued that the process of radiation would continue until the black hole had evaporated completely. At the end of this process, all the initial energy in the black hole would have been transferred to the radiation. But, according to Hawking's argument, the radiation would retain no information about the initial state and therefore information about the initial state would be lost.

More specifically, Hawking argued that the pattern of radiation emitted from the black hole would be random, with a probability distribution controlled only by the black hole's initial temperature, charge, and angular momentum, not by the initial state of the collapse. The state produced by such a probabilistic process is called a mixed state in quantum mechanics. Therefore, Hawking argued that if the star or material that collapsed to form the black hole started in a specific pure quantum state, the process of evaporation would transform the pure state into a mixed state. This is inconsistent with the unitarity of quantum-mechanical evolution discussed above.

The loss of information can be quantified in terms of the change in the fine-grained von Neumann entropy of the state. A pure state is assigned a von Neumann entropy of 0, whereas a mixed state has a finite entropy. The unitary evolution of a state according to Schrödinger's equation preserves the entropy. Therefore Hawking's argument suggests that the process of black-hole evaporation cannot be described within the framework of unitary evolution. Although this paradox is often phrased in terms of quantum mechanics, the evolution from a pure state to a mixed state is also inconsistent with Liouville's theorem in classical physics (see e.g.[18]).

In equations, Hawking showed that if one denotes the creation and annihilation operators at a frequency  ω {\displaystyle \omega } for a quantum field propagating in the black-hole background by  a ω {\displaystyle a_{\omega }} and  a ω † {\displaystyle a_{\omega }^{\dagger }} then the expectation value of the product of these operators in the state formed by the collapse of a black hole would satisfy  ⟨ a ω a ω † ⟩ h a w k = 1 1 − e − ω / k T {\displaystyle \langle a_{\omega }a_{\omega }^{\dagger }\rangle _{\rm {hawk}}={1 \over 1-e^{-\omega /{kT}}}} where k is the Boltzmann constant and T is the temperature of the black hole. (See, for example, section 2.2 of.[9]) This formula has two important aspects. The first is that the form of the radiation depends only on a single parameter, temperature, even though the initial state of the black hole cannot be characterized by one parameter. Second, the formula implies that the black hole radiates mass at a rate given by  d M d t = − a T 4 {\displaystyle {dM \over dt}=-{aT^{4}}} where a is constant related to fundamental constants, including the Stefan–Boltzmann constant and certain properties of the black hole spacetime called its greybody factors.

The temperature of the black hole is in turn dependent on its mass, charge, and angular momentum. For a Schwarzschild Black Hole the temperature is given by  T = ℏ c 3 8 π k G M {\displaystyle T={\hbar c^{3} \over 8\pi kGM}} This means that if the black hole starts out with an initial mass  M 0 {\displaystyle M_{0}} , it evaporates completely in a time proportional to  M 0 3 {\displaystyle M_{0}^{3}} .

The important aspect of these formulas is that they suggest that the final gas of radiation formed through this process depends only on the black hole's temperature and is independent of other details of the initial state. This leads to the following paradox. Consider two distinct initial states that collapse to form a Schwarzschild black hole of the same mass. Even though the states were distinct at first, since the mass (and hence the temperature) of the black holes is the same, they will emit the same Hawking radiation. Once they evaporate completely, in both cases, one will be left with a featureless gas of radiation. This gas cannot be used to distinguish between the two initial states, and therefore information has been lost.

### Page curve

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During the same time period in the 1970s, Don Page was a doctoral student of Stephen Hawking. He objected to Hawking's reasoning leading to the paradox above, initially on the basis of violation of CPT symmetry.[19] In 1993, Page focused on the combined system of a black hole with its Hawking radiation as one entangled system, a bipartite system, evolving over the lifetime of the black hole evaporation. Lacking the ability to make a full quantum analysis, he nonetheless made a powerful observation: If a black hole starts in a pure quantum state and evaporates completely by a unitary process, the von Neumann entropy or entanglement entropy of the Hawking radiation initially increases from zero and then must decrease back to zero when the black hole to which the radiation is entangled has totally evaporated.[5] This is known as the Page curve; and the time corresponding to the maximum or turnover point of the curve, which occurs at about half the black-hole lifetime, is called the Page time.[20] In short, if black hole evaporation is unitary, then the radiation entanglement entropy follows the Page curve. After the Page time, correlations appear and the radiation becomes increasingly information rich.[6]

Recent progress in deriving the Page curve for unitary black hole evaporation is a significant step towards finding both a resolution to the information paradox and a more general understanding of unitarity in quantum gravity.[21] Many researchers consider deriving the Page curve as synonymous with solving the black hole information paradox.[10]: 291

## Popular culture

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The information paradox has received coverage in the popular media and has been described in popular-science books. Some of this coverage resulted from a widely publicized bet made in 1997 between John Preskill on the one hand with Hawking and Kip Thorne on the other that information was not lost in black holes. The scientific debate on the paradox was described in Leonard Susskind's 2008 book The Black Hole War. (The book carefully notes that the 'war' was purely a scientific one, and that, at a personal level, the participants remained friends.[22]) Susskind writes that Hawking was eventually persuaded that black-hole evaporation was unitary by the holographic principle, which was first proposed by 't Hooft, further developed by Susskind, and later given a precise string theory interpretation by the AdS/CFT correspondence.[23] In 2004, Hawking also conceded the 1997 bet, paying Preskill with a baseball encyclopedia "from which information can be retrieved at will". Thorne refused to concede.[24]

## Solutions

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Since the 1997 proposal of the AdS/CFT correspondence, the predominant belief among physicists is that information is indeed preserved in black hole evaporation. There are broadly two main streams of thought about how this happens. Within what might broadly be termed the "string theory community", the dominant idea is that Hawking radiation is not precisely thermal but receives quantum correlations that encode information about the black hole's interior.[9] This viewpoint has been the subject of extensive recent research and 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.[25][26] Hawking himself was influenced by this view and in 2004 published a paper that assumed the AdS/CFT correspondence and argued that quantum perturbations of the event horizon could allow information to escape from a black hole, which would resolve the information paradox.[27] In this perspective, it is the event horizon of the black hole that is important and not the black-hole singularity. The GISR (Gravity Induced Spontaneous Radiation) mechanism of references[28][29] can be considered an implementation of this idea but with the quantum perturbations of the event horizon replaced by the microscopic states of the black hole.

On the other hand, within what might broadly be termed the "loop quantum gravity community", the dominant belief is that to resolve the information paradox, it is important to understand how the black-hole singularity is resolved. These scenarios are broadly called remnant scenarios since information does not emerge gradually but remains in the black-hole interior only to emerge at the end of black-hole evaporation.[12]

Researchers also study other possibilities, including a modification of the laws of quantum mechanics to allow for non-unitary time evolution.

Some of these solutions are described at greater length below.

### GISR mechanism resolution to the paradox

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This resolution takes GISR as the underlying mechanism for Hawking radiation, considering the latter only as a resultant effect. The physics ingredients of GISR are reflected in the following explicitly hermitian hamiltonian

H = ( w i w − j ⋱ 0 1 ) + ∑ q ℏ ω q a q † a q + ∑ u , v | u − v | = ℏ ω q g u n v ℓ b u n v ℓ † a q g u n v ℓ ∝ − ℏ G { M u , M v } m a x S i m l { Ψ [ M u n ( r ) ] , Ψ [ M v ℓ ( r ) ] } {\displaystyle {\begin{aligned}H&={\begin{pmatrix}w^{i}\\\&w_{-}^{j}\\\&&\ddots \\\&&&{\scriptstyle {\it {0}}}^{\scriptscriptstyle {\it {1}}}\end{pmatrix}}+\sum _{q}\hbar \omega _{q}a_{q}^{\dagger }a_{q}+\sum _{u,v}^{|u-v|=\hbar \omega _{q}}g_{u^{n}v^{\ell }}b_{u^{n}v^{\ell }}^{\dagger }a_{q}\\\g_{u\;\\!\\!^{n}v^{\ell }}&\propto -{\frac {\hbar }{G\\{M_{u},M_{v}\\}^{\mathrm {max} }}}\mathrm {Siml} \\{\Psi [M_{u\;\\!\\!^{n}}\\!(r)],\Psi [M_{v\;\\!\\!^{\ell }}\\!(r)]\\}\end{aligned}}}

The first term of  H {\displaystyle H} is a diagonal matrix representing the microscopic state of black holes no heavier than the initial one. The second term describes vacuum fluctuations of particles around the black hole and is represented by many harmonic oscillators. The third term couples the vacuum fluctuation modes to the black hole, such that for each mode whose energy matches the difference between two states of the black hole, the latter transitions with an amplitude proportional to the similarity factor of their microscopic wave functions. Transitions between higher energy state  u {\displaystyle u} to lower energy state  v {\displaystyle v} and vice versa, are equally permitted at the Hamiltonian level. This coupling mimics the photon-atom coupling in the Jaynes–Cummings model of atomic physics, replacing the photon's vector potential with the binding energy of particles to be radiated in the black hole case, and the dipole moment of initial-to-final state transitions in atoms with the similarity factor of the initial and final states' wave functions in black holes. Despite its ad hoc nature, this coupling introduces no new interactions beyond gravity, and it is deemed necessary irrespective of the future development of quantum gravitational theories.

From the hamiltonian of GISR and the standard Schrodinger equation controlling the evolution of wave function of the system

| ψ ( t ) ⟩ = ∑ u = w 0 ∑ n = 1 u ∑ ω s ω + u = w e − i u t − i ω t c u n ω s ( t ) | u n ⊗ ω s ⟩ {\displaystyle |\psi (t)\rangle =\sum _{u=w}^{0}\sum _{n=1}^{u}\sum _{\omega {}s}^{\omega +u=w}e^{-iut-i\omega {}t}c_{u\;\\!\\!^{n}}^{\omega {}s}(t)|u\;\\!\\!^{n}\otimes \omega {}s\rangle }

i ℏ ∂ t | ψ ( t ) ⟩ = H | ψ ( t ) ⟩ {\displaystyle i\hbar {\partial }_{t}|\psi (t)\rangle =H|\psi (t)\rangle }

here  ω s {\displaystyle \omega {}s} is the index of the radiated particles set with total energy  ω {\displaystyle \omega } . In the case of short time evolution or single quantum emission, Wigner-Wiesskopf approximation allows one[28][29] to show that the power spectrum of GISR is exactly of thermal type and the corresponding temperature equals that of Hawking radiation. However, in the case of long time evolution or continuous quantum emission, the process is off-equilibrium and is characterised by an initial state dependent black hole mass or temperature vs. time curve. The observers far away can retrieve the information stored in the initial black hole from this mass or temperature versus time curve.

The hamiltonian and wave function description of GISR allows one to calculate the entanglement entropy between the black hole and its Hawking particles explicitly.

s B R = − tr B ⁡ ρ B log ⁡ ρ B = − t r R ρ R log ⁡ ρ R {\displaystyle s_{BR}=-\operatorname {tr} _{B}\rho _{B}\log \rho _{B}=-tr_{R}\rho _{R}\log \rho _{R}}

ρ B = tr R ⁡ ∑ u = w 0 ∑ n = 1 u ∑ ω s ω + u = w | c u n ω s ⟩ ⟨ c u n ω s | {\displaystyle \rho _{B}=\operatorname {tr} _{R}\sum _{u=w}^{0}\sum _{n=1}^{u}\sum _{\omega {}s}^{\omega +u=w}|c_{u^{n}}^{\omega {}s}\rangle \langle c_{u^{n}}^{\omega {}s}|}

ρ R = tr B ⁡ ∑ u = w 0 ∑ n = 1 u ∑ ω s ω + u = w | c u n ω s ⟩ ⟨ c u n ω s | {\displaystyle \rho _{R}=\operatorname {tr} _{B}\sum _{u=w}^{0}\sum _{n=1}^{u}\sum _{\omega {}s}^{\omega +u=w}|c_{u^{n}}^{\omega {}s}\rangle \langle c_{u^{n}}^{\omega {}s}|}

Since the Hamiltonian of GISR is explicitly Hermitian, the resulting Page curve is naturally expected, except for some late-time Rabi-type oscillations. These oscillations arise from the equal probability of emission and absorption transitions as the black hole approaches the vanishing stage. The most important lesson from this calculation is that the intermediate state of an evaporating black hole cannot be considered a semiclassical object with a time-dependent mass. Instead, it must be viewed as a superposition of many different mass ratio combinations of the black hole and Hawking particles. References[28][29] designed a Schrödinger cat-type thought experiment to illustrate this fact, where an initial black hole is bounded with a group of living cats and each Hawking particle kills one from the group. In the quantum description, because the exact timing and number of particles radiated by a black hole cannot be determined definitively, the intermediate state of the evaporating black hole must be considered a superposition of many cat groups, each with a different ratio of dead members. The biggest flaw in the argument for the information loss paradox is ignoring this superposition.

### Small-corrections resolution to the paradox

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This idea suggests that Hawking's computation fails to keep track of small corrections that are eventually sufficient to preserve information about the initial state.[30][31][9] This can be thought of as analogous to what happens during the mundane process of "burning": the radiation produced appears to be thermal, but its fine-grained features encode the precise details of the object that was burnt. This idea is consistent with reversibility, as required by quantum mechanics. It is the dominant idea in what might broadly be termed the string-theory approach to quantum gravity.

More precisely, this line of resolution suggests that Hawking's computation is corrected so that the two point correlator computed by Hawking and described above becomes  ⟨ a ω a ω † ⟩ e x a c t = ⟨ a ω a ω † ⟩ h a w k ( 1 + ϵ 2 ) {\displaystyle \langle a_{\omega }a_{\omega }^{\dagger }\rangle _{\rm {exact}}=\langle a_{\omega }a_{\omega }^{\dagger }\rangle _{\rm {hawk}}(1+\epsilon _{2})} and higher-point correlators are similarly corrected  ⟨ a ω 1 a ω 1 † a ω 2 a ω 2 † … a ω n a ω n † ⟩ e x a c t = ⟨ a ω a ω † ⟩ h a w k ( 1 + ϵ n ) {\displaystyle \langle a_{\omega _{1}}a_{\omega _{1}}^{\dagger }a_{\omega _{2}}a_{\omega _{2}}^{\dagger }\ldots a_{\omega _{n}}a_{\omega _{n}}^{\dagger }\rangle _{\rm {exact}}=\langle a_{\omega }a_{\omega }^{\dagger }\rangle _{\rm {hawk}}(1+\epsilon _{n})} The equations above utilize a concise notation and the correction factors  ϵ i {\displaystyle \epsilon _{i}} may depend on the temperature, the frequencies of the operators that enter the correlation function and other details of the black hole.

Maldacena initially explored such corrections in a simple version of the paradox.[32] They were then analyzed by Papadodimas and Raju,[33][34][35] who showed that corrections to low-point correlators (such as  ϵ 2 {\displaystyle \epsilon _{2}} above ) that were exponentially suppressed in the black-hole entropy were sufficient to preserve unitarity, and significant corrections were required only for very high-point correlators. The mechanism that allowed the right small corrections to form was initially postulated in terms of a loss of exact locality in quantum gravity so that the black-hole interior and the radiation were described by the same degrees of freedom. Recent developments suggest that such a mechanism can be realized precisely within semiclassical gravity and allows information to escape.[8] See § Recent developments.

### Fuzzball resolution to the paradox

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Some researchers, most notably Samir Mathur, have argued[11] that the small corrections required to preserve information cannot be obtained while preserving the semiclassical form of the black-hole interior and instead require a modification of the black-hole geometry to a fuzzball.[36][37][38]

The defining characteristic of the fuzzball is that it has structure at the horizon scale. This should be contrasted with the conventional picture of the black-hole interior as a largely featureless region of space. For a large enough black hole, tidal effects are very small at the black-hole horizon and remain small in the interior until one approaches the black-hole singularity. Therefore, in the conventional picture, an observer who crosses the horizon may not even realize they have done so until they start approaching the singularity. In contrast, the fuzzball proposal suggests that the black hole horizon is not empty. Consequently, it is also not information-free, since the details of the structure at the surface of the horizon preserve information about the black hole's initial state. This structure also affects the outgoing Hawking radiation and thereby allows information to escape from the fuzzball.

The fuzzball proposal is supported by the existence of a large number of gravitational solutions called microstate geometries.[39][40][41][42][43]

The firewall proposal can be thought of as a variant of the fuzzball proposal that posits that the black-hole interior is replaced by a firewall rather than a fuzzball. Operationally, the difference between the fuzzball and the firewall proposals has to do with whether an observer crossing the horizon of the black hole encounters high-energy matter, suggested by the firewall proposal, or merely low-energy structure, suggested by the fuzzball proposal. The firewall proposal also originated with an exploration of Mathur's argument that small corrections are insufficient to resolve the information paradox.[11]

The fuzzball and firewall proposals have been questioned for lacking an appropriate mechanism that can generate structure at the horizon scale.[9]

### Strong-quantum-effects resolution to the paradox

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In the final stages of black-hole evaporation, quantum effects become important and cannot be ignored. The precise understanding of this phase of black-hole evaporation requires a complete theory of quantum gravity. Within what might be termed the loop-quantum-gravity approach to black holes, it is believed that understanding this phase of evaporation is crucial to resolving the information paradox.

This perspective holds that Hawking's computation is reliable until the final stages of black-hole evaporation, when information suddenly escapes.[30][31][44][12] Another possibility along the same lines is that black-hole evaporation simply stops when the black hole becomes Planck-sized. Such scenarios are called "remnant scenarios".[30][31]

An appealing aspect of this perspective is that 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. On the other hand, this idea implies that just before the sudden escape of information, a very small black hole must be able to store an arbitrary amount of information and have a very large number of internal states. Therefore, researchers who follow this idea must take care to avoid the common criticism of remnant-type scenarios, which is that they might may violate the Bekenstein bound and lead to a violation of effective field theory due to the production of remnants as virtual particles in ordinary scattering events.[45][46]

### Soft-hair resolution to the paradox

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In 2016, Hawking, Perry and Strominger noted that black holes must contain "soft hair".[47][48][49] Particles that have no rest mass, like photons and gravitons, can exist with arbitrarily low-energy and are called soft particles. The soft-hair resolution posits that information about the initial state is stored in such soft particles. The existence of such soft hair is a peculiarity of four-dimensional asymptotically flat space and therefore this resolution to the paradox does not carry over to black holes in Anti-de Sitter space or black holes in other dimensions.

### Information is irretrievably lost

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A minority view in the theoretical physics community is that information is genuinely lost when black holes form and evaporate.[30][31] This conclusion follows if one assumes that the predictions of semiclassical gravity and the causal structure of the black-hole spacetime are exact.

But this conclusion leads to the loss of unitarity. Banks, Susskind and Peskin argue that, in some cases, loss of unitarity also implies violation of energy–momentum conservation or locality, but this argument may possibly be evaded in systems with a large number of degrees of freedom.[50] 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 Penrose advocates critically depends on the condition that information is in fact lost in black holes. This new cosmological model might 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.[51] The significance of these findings was debated.[52][53][54][55]

Along similar lines, Modak, Ortíz, Peña, and Sudarsky have argued that the paradox can be dissolved by invoking foundational issues of quantum theory often called the measurement problem of quantum mechanics.[56] This work built on an earlier proposal by Okon and Sudarsky on the benefits of objective collapse theory in a much broader context.[57] The original motivation of these studies was Penrose's long-standing proposal wherein collapse of the wave-function is said to be inevitable in the presence of black holes (and even under the influence of gravitational field).[58][59] Experimental verification of collapse theories is an ongoing effort.[60]

### Other proposed resolutions

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Some other resolutions to the paradox have also been explored. These are listed briefly below.

* Information is stored in a large remnant[61][62]

This idea suggests that Hawking radiation stops before the black hole reaches the Planck size. Since the black hole never evaporates, information about its initial state can remain inside the black hole and the paradox disappears. But there is no accepted mechanism that would allow Hawking radiation to stop while the black hole remains macroscopic.
* Information is stored in a baby universe that separates from our own universe.[31][63]

Some models of gravity, such as the Einstein–Cartan theory of gravity, which extends general relativity to matter with intrinsic angular momentum (spin), predict the formation of such baby universes. No violation of known general principles of physics is needed. There are no physical constraints on the number of the universes, even though only one remains observable.

The Einstein-Cartan theory is difficult to test 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[64][65]

The final-state proposal[66] suggests that boundary conditions must be imposed at the black-hole singularity, which, from a causal perspective, is to the future of all events in the black-hole interior. This helps reconcile black-hole evaporation with unitarity but contradicts the intuitive idea of causality and locality of time-evolution.
* Quantum-channel theory

In 2014, Chris Adami argued that analysis using quantum channel theory causes any apparent paradox to disappear; Adami rejects black hole complementarity, arguing instead that no space-like surface contains duplicated quantum information.[67][68]
* Topological Invariants and Recursive Dynamics[69]

The K-Line Theory offers a novel resolution to the black hole information paradox through a framework based on recursive state evolution, topological invariant dynamics, and probabilistic equivalence. By employing symmetry indices and dynamic constants, the theory ensures that information is preserved throughout the black hole's lifecycle, including during its evaporation via Hawking radiation. Unlike previous proposals, which often fail to provide a mechanism for information preservation without introducing confounding drawbacks, K-Line Theory addresses these issues by maintaining a hierarchical structure of states and encoding quantum correlations coherently. Numerical simulations within the K-Line framework produce entropy behaviours consistent with the Page curve, demonstrating information retrieval and coherence. This approach bridges quantum mechanics and general relativity without violating established physical principles, providing a comprehensive mechanism for information conservation in black hole physics.

## Recent developments

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Significant progress was made in 2019, when, starting with work by Penington[70] and Almheiri, Engelhardt, Marolf and Maxfield,[71] researchers were able to compute the von Neumann entropy of the radiation black holes emit in specific models of quantum gravity.[8][25][26][72] These calculations showed that, in these models, the entropy of this radiation first rises and then falls back to zero. As explained above, one way to frame the information paradox is that Hawking's calculation appears to show that the von Neumann entropy of Hawking radiation increases throughout the lifetime of the black hole. But if the black hole formed from a pure state with zero entropy, unitarity implies that the entropy of the Hawking radiation must decrease back to zero once the black hole evaporates completely, i.e., the Page curve.[6] Therefore, the results above provide a resolution to the information paradox, at least in the specific models of gravity considered in these models.

These calculations compute the entropy by first analytically continuing the spacetime to a Euclidean spacetime and then using the replica trick. The path integral that computes the entropy receives contributions from novel Euclidean configurations called "replica wormholes". (These wormholes exist in a Wick rotated spacetime and should not be conflated with wormholes in the original spacetime.) The inclusion of these wormhole geometries in the computation prevents the entropy from increasing indefinitely.[7]

These calculations also imply that 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 provides evidence for the physical picture suggested by the ER=EPR proposal,[7] black hole complementarity, and the Papadodimas–Raju proposal.

It has been noted that the models used to perform the Page curve computations above have consistently involved theories where the graviton has mass, unlike the real world, where the graviton is massless.[73] These models have also involved a "nongravitational bath", which can be thought of as an artificial interface where gravity ceases to act. It has also been argued that a key technique used in the Page-curve computations, the "island proposal", is inconsistent in standard theories of gravity with a Gauss law.[74] This would suggest that the Page curve computations are inapplicable to realistic black holes and work only in special toy models of gravity. The validity of these criticisms remains under investigation; there is no consensus in the research community.[75][76]

In 2020, Laddha, Prabhu, Raju, and Shrivastava argued that, as a result of the effects of quantum gravity, information should always be available outside the black hole.[77] This would imply that the von Neumann entropy of the region outside the black hole always remains zero, as opposed to the proposal above, where the von Neumann entropy first rises and then falls. Extending this, Raju argued that Hawking's error was to assume that the region outside the black hole would have no information about its interior. [78]

Hawking formalized this assumption in terms of a "principle of ignorance".[2] The principle of ignorance is correct in classical gravity, when quantum-mechanical effects are neglected, by virtue of the no-hair theorem. It is also correct when only quantum-mechanical effects are considered and gravitational effects are neglected. But Raju argued that when both quantum mechanical and gravitational effects are accounted for, the principle of ignorance should be replaced by a "principle of holography of information"[9] that would imply just the opposite: all the information about the interior can be regained from the exterior through suitably precise measurements.

The two recent resolutions of the information paradox described above—via replica wormholes and the holography of information—share the feature that observables in the black-hole interior also describe observables far from the black hole. This implies a loss of exact locality in quantum gravity. Although this loss of locality is very small, it persists over large distance scales. This feature has been challenged by some researchers.[79]

## See also

[edit]

* 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
* No-hiding theorem
* Thorne–Hawking–Preskill bet

## References

[edit]

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## External links

[edit]

* Black Hole Information Loss Problem, a USENET physics FAQ page
* Preskill, John (1992). "Do black holes destroy information?". arXiv:hep-th/9209058.. Discusses methods of attack on the problem, and their apparent shortcomings.
* Peplow, Mark (2004). "Hawking changes his mind about black holes". Nature. doi:10.1038/news040712-12. Report on Hawking's 2004 theory in Nature.
* Hawking, S. W. (2005). "Information loss in black holes". Physical Review D. 72 (8): 084013. arXiv:hep-th/0507171. Bibcode:2005PhRvD..72h4013H. doi:10.1103/PhysRevD.72.084013. S2CID 118893360. Stephen Hawking's purported solution to the black hole unitarity paradox.
* Hawking and unitarity: a July 2005 discussion of the information loss paradox and Stephen Hawking's role in it
* The Hawking Paradox - BBC Horizon documentary (2005)
* "Horizon" The Hawking Paradox at IMDb
* A Black Hole Mystery Wrapped in a Firewall Paradox

* v
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Black holes

* Outline

Types|

* BTZ black hole
* Schwarzschild
* Rotating
* Charged
* Virtual
* Kugelblitz
* Supermassive
* Primordial
* Direct collapse
* Rogue
* Malament–Hogarth spacetime

Size|

* Micro
* Extremal
* Electron
* Stellar
* Microquasar
* Intermediate-mass
* Supermassive
* Active galactic nucleus
* Quasar
* LQG
* Blazar
* OVV

Formation|

* Stellar evolution
* Gravitational collapse
* Neutron star
* Related links
* Tolman–Oppenheimer–Volkoff limit
* White dwarf
* Related links
* Supernova
* Micronova
* Hypernova
* Related links
* Gamma-ray burst
* Binary black hole
* Quark star
* Supermassive star
* Quasi-star
* Supermassive dark star
* X-ray binary

Properties|

* Astrophysical jet
* Gravitational singularity
* Ring singularity
* Theorems
* Event horizon
* Photon sphere
* Innermost stable circular orbit
* Ergosphere
* Penrose process
* Blandford–Znajek process
* Accretion disk
* Hawking radiation
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* M–sigma relation
* Quasi-periodic oscillation
* Thermodynamics
* Bekenstein bound
* Bousso's holographic bound
* 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
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* Planck star
* Q star
* Fuzzball
* Geon

Analogs|

* Optical black hole
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Lists|

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Related|

* Outline of black holes
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* Black holes in fiction
* Big Bang
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* Compact star
* Exotic star
* Quark star
* Preon star
* Gravitational waves
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* Gravity well
* Hypercompact stellar system
* Membrane paradigm
* Naked singularity
* Population III star
* Supermassive star
* Quasi-star
* Supermassive dark star
* Rossi X-ray Timing Explorer
* Superluminal motion
* Timeline of black hole physics
* White hole
* Wormhole
* Tidal disruption event
* Planet Nine

Notable|

* Cygnus X-1
* XTE J1650-500
* XTE J1118+480
* A0620-00
* Sagittarius A*
* Centaurus A
* Phoenix Cluster
* PKS 1302-102
* OJ 287
* SDSS J0849+1114
* TON 618
* MS 0735.6+7421
* NeVe 1
* Hercules A
* 3C 273
* Q0906+6930
* Markarian 501
* ULAS J1342+0928
* PSO J030947.49+271757.31
* AT2018hyz
* Swift J1644+57
* 1ES 1927+654

* Category
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Quantum gravity

Central concepts|

* AdS/CFT correspondence
* Batalin–Vilkovisky formalism
* CA-duality
* Causal patch
* Faddeev–Popov ghost
* Gravitational anomaly
* Graviton
* Holographic principle
* IR/UV mixing
* Planck units
* Quantum foam
* Ryu–Takayanagi conjecture
* Trans-Planckian problem
* Weinberg–Witten theorem

Toy models|

* 2+1D topological gravity
* CGHS model
* Jackiw-Teitelboim gravity
* Liouville gravity
* RST model
* Topological quantum field theory

Quantum field theory
in curved spacetime|

* Bunch–Davies vacuum
* Hawking radiation
* Semiclassical gravity
* Unruh effect

Black holes|

* Black hole complementarity
* Black hole information paradox
* Black-hole thermodynamics
* Bekenstein bound
* Bousso's holographic bound
* Cosmic censorship hypothesis
* ER = EPR
* Firewall (physics)
* Gravitational singularity

Approaches|

| String theory|

* Bosonic string theory
* M-theory
* Supergravity
* Superstring theory

|

Canonical quantum gravity|

* Loop quantum gravity
* Wheeler-DeWitt equation

Euclidean quantum gravity|

* Hartle-Hawking state

Others|

* Causal dynamical triangulation
* Causal sets
* Dual graviton
* Group field theory
* Noncommutative geometry
* Spin foam
* Superfluid vacuum theory
* Twistor theory

Applications|

* Quantum cosmology
* Eternal inflation
* FRW/CFT duality
* Multiverse

See also: Template:Quantum mechanics topics

* v
* t
* e

Stephen Hawking

Physics|

* Hawking radiation
* Black hole thermodynamics
* Micro black hole
* Chronology protection conjecture
* Gibbons–Hawking ansatz
* Gibbons–Hawking effect
* Gibbons–Hawking space
* Gibbons–Hawking–York boundary term
* Hartle–Hawking state
* Penrose–Hawking singularity theorems
* Hawking energy

Books|

| Science|

* The Large Scale Structure of Space–Time (1973)
* A Brief History of Time (1988)
* Black Holes and Baby Universes and Other Essays (1993)
* The Nature of Space and Time (1996)
* The Universe in a Nutshell (2001)
* On the Shoulders of Giants (2002)
* A Briefer History of Time (2005)
* God Created the Integers (2005)
* The Grand Design (2010)
* The Dreams That Stuff Is Made Of (2011)
* Brief Answers to the Big Questions (2018)
* On the Origin of Time (2023, posthume message)

|

Fiction|

* George's Secret Key to the Universe (2007)
* George's Cosmic Treasure Hunt (2009)
* George and the Big Bang (2011)
* George and the Unbreakable Code (2014)
* George and the Blue Moon (2016)
* Unlocking the Universe (2020)

Memoirs|

* My Brief History (2013)

Films|

* A Brief History of Time (1991)
* Hawking (2004)
* Hawking (2013)
* The Theory of Everything (2014)

Television|

* God, the Universe and Everything Else (1988)
* Stephen Hawking's Universe (1997 documentary)
* Stephen Hawking: Master of the Universe (2008 documentary)
* Genius of Britain (2010 series)
* Into the Universe with Stephen Hawking (2010 series)
* Brave New World with Stephen Hawking (2011 series)
* Genius by Stephen Hawking (2016 series)

Family|

* Jane Wilde Hawking (first wife)
* Lucy Hawking (daughter)

Other|

* In popular culture
* Namesakes
* Black hole information paradox
* Thorne–Hawking–Preskill bet

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