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Teleporting entanglement during black hole evaporation

The unitary evaporation of a black hole (BH) in an initially pure state must lead to the eventual purification of the emitted radiation. It follows that the late radiation has to be entangled with the early radiation and, as a consequence, the entanglement among the Hawking pair partners has to decrease continuously from maximal to vanishing during the BH's life span. Starting from the basic premise that both the horizon radius and the center of mass of a finite-mass BH are fluctuating quantum mechanically, we show how this process is realized. First, it is shown that the horizon fluctuations induce a small amount of variance in the total linear momentum of each created pair. This is in contrast to the case of an infinitely massive BH, for which the total momentum of the produced pair vanishes exactly on account of momentum conservation. This variance leads to a random recoil of the BH during each emission and, as a result, the center of mass of the BH undergoes a quantum random walk. Consequently, the uncertainty in its momentum grows as the square root of the number of emissions. We then show that this uncertainty controls the amount of deviation from maximal entanglement of the produced pairs and that this deviation is determined by the ratio of the cumulative number of emitted particles to the initial BH entropy. Thus, the interplay between the horizon and center-of-mass fluctuations provides a mechanism for teleporting entanglement from the pair partners to the BH and the emitted radiation.


Introduction
Let us consider an evaporating black hole (BH) in a four-dimensional asymptotically flat spacetime. The standard Hawking description of BH radiation via pair production [1,2] implies that the quantum state of the near-horizon matter is the Unruh vacuum state, which is that of maximally entangled pairs straddling the horizon. Ultimately, the positive-energy partners fly off to become the Hawking radiation, while their negative-energy counterparts fall into the interior and lead to a reduction in the BH mass.
One problem with this picture is its failure to explain how information can escape from the BH, which is an essential requirement for a unitary process of evaporation. It was long thought that this quandary could be resolved by non-perturbative effects such as contributions from other geometries [3] or subtle correlations between the emitted quanta [4]. However, this optimistic stance leads one to an even bigger issue: Explaining how the information can get out without violating another fundamental tenet of quantum theory -the monogamy of entanglement, i.e., that no particle can be strongly entangled with more than one other particle. This concern has been championed by Mathur [5,6,7,8,10], while Almheiri et. al. brought this matter to the forefront with their notion of a near-horizon "firewall" [11] (also see [12,13,14,15,16]).
Using the strong-subadditivity inequality, one can recast this problem in precise terms, but it is also easy to understand the cen-tral issues at a simple intuitive level. For information to escape from the BH and then be encoded in the state of the external radiation, there must be some degree of entanglement between the emitted Hawking particles. Otherwise, the final state of the radiation could have no "knowledge" about the initial state of the collapsing matter. Also, it is not viable for this information to be released only in the final stages of evaporation, as the amount that is stored in the BH interior cannot exceed the horizon area in Planck units. To argue differently would be to argue for BH remnants. Monogamy of entanglement then rules out the possibility of maximally entangled pairs in the near-horizon zone -the Unruh state cannot be the correct quantum state of the near-horizon matter.
One might hope that the entanglement between pair partners could be large enough that the state is still "approximately Unruh". However, this hope is squashed once the BH reaches its half life in terms of the number of the emitted particles, the so-called Page time. The reason being that, according to the Page model of BH evaporation [17], which establishes parametrically the minimal rate of information release for a unitary process, this is the time when information must begin to emerge from the BH at a rate of order unity. This, in turn, implies that the near-horizon state has significant corrections away from the Unruh state.
The Unruh state had always been given preferential status in this context because a freely falling observer in this state would fall according to the predictions of classical general relativity. A different choice of vacuum would lead to deviations from these predictions, and it is implicitly assumed by many that such a choice would be problematic; for example, by putting the validity of Einstein's equivalence principle at risk. We do not agree, however, that the demise of the equivalence principle follows as a inevitable consequence of having disentangled pairs [18,19]. In particular, it is shown in [19] that, for typical objects, the classical tidal forces at the horizon of a finite-mass BH are more dangerous than a significant degree of disentanglement. Our conclusion is that one cannot use this line of reasoning to single out the Unruh vacuum as the preferred state, and we will proceed to consider other possibilities in this spirit.
Our basic premise is that a consistent treatment of a finitemass BH must account for its quantum fluctuations [20,21]. The location of the BH horizon is, at least in principle, a physically measurable quantity [22], so that it makes sense to talk about its quantum fluctuations. Similarly for the position and momentum of the BH center of mass, and so their quantum spreads also have a physical meaning. So far, we have considered the impact of fluctuations of the horizon area (or radius) on the BH evaporation process [23,24,25]. But, as mentioned, the center of mass of the BH is also fluctuating quantum mechanically.
The main new idea of the current paper is that the interplay between the quantum fluctuations of the horizon and those of the center of mass determine the state of the produced pairs, while allowing for the swapping or teleportation of entanglement from the pair partners to the BH and emitted Hawking radiation. Our focus is on the entanglement of linear momentum, but we do expect that similar considerations also apply to angular momentum.
In Hawking's model for pair production [2], the negative-energy partner is subsumed by the BH interior and the positive-energy partner escapes to the exterior. At times much earlier than the Page time, the pair is in a state that is close to maximally entangled. As the partnership ends with the subsumption of the negative-energy partner, the state of the BH interior will have to change accordingly. It is unclear what the state of the BH interior is to begin with (however, see [26,27]), never mind what it will change into. But we do know that unitary evolution implies that entanglement will not be destroyed, only teleported.
Hence, it must be that the BH interior is now entangled with the positive-energy partner, which is by then part of the exterior radiation.
Ultimately, the BH must teleport this newly acquired entanglement to its exterior; otherwise, the purification of the external radiation cannot be completed. The only means that the BH has for doing this is through the influence of its near-horizon gravitational field on subsequently produced pairs. So, somehow, the pair-production mechanism needs to "remember" the history of emissions! But how? On one hand, the state of the produced pairs is apparently determined solely by the gravitational field near the horizon of the BH. On the other, a "memory" requires a dynamical mechanism that allows the history of emissions to change the state of the produced pairs.
Our proposal 1 is that the swapping or teleportation of entanglement proceeds via the transfer of quantum fluctuations; from those of the horizon to those of the center of mass.
In the limiting case, when the BH mass is taken to infinity, First, we will show that the horizon fluctuations induce a small variance in the total momentum of each of the created pairs. This variance results in a random recoil of the BH; its center-ofmass momentum becomes uncertain by a small amount during each emission, and these deviations accumulate. The resulting picture is that the center-of-mass momentum of the BH undergoes 1 A similar idea concerning angular momentum was discussed for the case of a rotating BH by Chowdhury and Mathur [28] in the context of fuzzball models. a quantum random walk with (approximately) fixed step sizes and, hence, the uncertainty in its momentum grows as the square root of the number of emissions. The growing uncertainty in the center-of-mass momentum leads to an increasing uncertainty in the correlation between the momenta of the pair partners, which in turn decreases their entanglement. What will eventually be shown is that this decrease in entanglement is determined by the ratio of the cumulative number of emitted particles to the initial BH entropy.
There are other sources of momentum fluctuations besides those induced by the horizon fluctuations. One source is the uncertainty principle. If the initial center-of-mass position of the BH is localized to within a region of size R S , then the center-of-mass momentum has to have a spread of order 1/R S [31]. An additional source is the random recoil of the BH due to the eventual absorption of the negative-energy partner of the emitted positive-energy Hawking particles. (See Sect. 6 of [7]. Also, [32,33].) This recoil is of order 1/R S per emitted particle. However, since momentum is conserved in this process, it does not lead to any change in the entanglement of the emitted pairs, in agreement with the conclusion of [7].

Entanglement in pair production
What are the entangled quantities in the BH pair-production?
They cannot be just the spin or angular momentum because one can imagine a situation when a Schwarzschild BH emits most of the radiation in the form of scalar particles. And just how entangled need they be?
We begin answering these questions by considering the physical observables in the pair-production process. The factor that determines the degree of entanglement between the produced par-ticles is the near-horizon gravitational field. For the case of electron-positron pair production, this is made clear in (e.g.) [34,35].
Suppose that one measures the momentum of an outgoing Let us set the initial momentum of the BH center of mass to zero, P CM = 0 . If the momentum of the first emitted particle is measured, we would know with high precision what the change to P CM would be. Meaning that, in this situation, the variables are maximally entangled and imply maximal entanglement between pair members. If, on the other hand, we measure the momentum of the second emitted particle but not the first, then P CM would only be known to accuracy l P /R 2 S since the kick from the first particle is unknown. Clearly, if we measure just the momentum of the N th emitted particle (after, say, about half the particles were emitted so that N ∼ S BH ), then P CM would only be known to an accuracy of about √ N lp It follows that we can write where Q N = N i q i = P CM (N + 1) and the Gaussian incorporates the growing uncertainty in the center-of-mass position due to its previously discussed random walk. As explained in Section 2, the width of this distribution is given by A reduced density matrix for the momentum of the N th pair can now be written in the standard way, for which a straightforward calculation reveals that We may now apply Eq. (4) Using Eq. (2), we obtain The purity is initially very small, indicating that the pairs are maximally entangled. As more particles are emitted, the purity increases until reaching N ∼ S BH (0) . Then the purity becomes order one, indicating that the pairs are produced effectively in a product state.
These observations can be made more formal by parametrizing the associated entropy. Following Mathur [9], one can define a parameter ǫ that indicates the deviation from maximal entanglement. In general, ǫ = Smax−S Smax , where S is some measure of entropy and S max is its maximal value. Mathur used the Von Neumann entropy, whereas we used the Rényi entropy in [37].
Different parametrizations will, of course, lead to somewhat different quantitative results.
In the current context, we find that the linear entropy S L is the appropriate measure of entanglement, being directly related to the purity of the reduced density matrix (e.g.) [36]. For a system with a large number of possible states, as in the case of momentum entanglement, the linear entropy is given by S L = 1 − Tr ρ 2 red . The linear entropy for the pairs is therefore given by As the linear entropy ranges from 1 (maximal entanglement) to 0 (product state), the deviation parameter for the N th produced pair is simply As expected, this parameter is initially very small and already of order unity at times comparable to the Page time but never exceeds unity.
One final consideration: As the entanglement between the pair partners decreases, the entanglement between the positive-energy partner and the previously emitted particles will increase in kind.
This is because the total momentum of all emitted particles must sum up to zero by the end of evaporation; so that, if we knew the momenta of the first N emissions, our knowledge of the N th particle's momentum would accordingly increase.
This latter entanglement also measures the amount of correlation between the N th emission and all the emissions that follow it until the end of the evaporation. This is because, if one measures the momenta of the first N emitted articles, then the sum of momenta of the rest of the S BH (0) − N particles has to be exactly of the same magnitude and opposite direction as the sum of the first N particles.
To make this idea precise, one can repeat the previous anal- q i . Then, as N grows, the variance of K CM (N) is decreasing in proportion to the decrease of the variance in P CM . It is also clear that q N is always maximally entangled with the sum P CM + K CM because q N + P CM + K CM = 0 .

Conclusion
We have relied on a pair of fundamental ideas -unitary evolution and the fact that a finite mass BH must fluctuate quantum mechanically -to conclude that the state of the near-horizon pairs is much different than the Unruh state at all but the earliest stages of BH evaporation. Mathur and others have deduced this outcome on the basis of general arguments; our contribution is to provide a physical mechanism that leads to such a state and to provide a quantitative treatment of its deviations from the Unruh vacuum. Our result is consistent with [37], where we found by using the constraint of strong subadditivity that N/S BH (0) is an upper bound on the degree of disentanglement.
A central lesson of our work is that deviations from maximal entanglement depend on the quantum fluctuations of a finite-mass BH. On the contrary, an infinitely massive object cannot recoil, assuring that momentum and, therefore, perfect entanglement are conserved for the produced pairs. This explains why Hawking and others concluded that the pairs were maximally entangled; given the assumption of an infinitely massive BH, this must be so.
The techniques that were used here have an element of crudeness, as do many model-independent calculations. One would like to further the analysis in a more rigorous way, but this requires a much clearer understanding about the state of the BH interior and, then, how it changes when a negative-energy particle is subsumed. We have only begun to broach the subject of the BH interior [27] but hope that this path eventually leads to calculations along these lines.

Acknowledgments
We would like to thank Samir Mathur for discussions. The re-

A Momentum entanglement
As a concrete example of momentum entanglement, we discuss the state of a pair of particles in 3 space dimensions. For simplicity, we consider a pair of massless bosons and, therefore, the state has to be symmetric under the exchange of the particles. Similar conclusions would be obtained for massive bosons or fermions.
The state of the pair can be written as and its density matrix is then so that the density-matrix elements are given by ρ( p 1 , p 2 ; q 1 , q 2 ) = g( p 1 , p 2 )g † ( q 2 , q 1 ) , and the reduced density-matrix elements are expressible as Given that the full density matrix is normalized, the reduced density matrix is as well, Tr gg † = 1 . One can use the Rényi entropy for estimating the amount of entanglement, H 2 = − ln Tr(ρ 2 red ) (Tr ρ red ) 2 = − ln Tr (gg † ) 2 . If the total momentum of the pair vanishes, then where N is a normalization factor (Tr 1 = N ). The Rényi entropy is then given by which indicates that the pair is maximally entangled. As expected, when the total momentum of the pair is fixed, the state of the pairs is indeed maximally entangled. On the other hand, if the state is a product state, with N 1 , N 2 being normalization factors, then H 2 = 0 as expected.
We now understand that, in order to deviate from maximal entanglement, there must be some spread in the total momentum of the pair. In technical terms, the matrix g( p 1 , p 2 ) has to have some support away from the diagonal. An example could be a Gaussian spread in the momentum difference with some small width σ < ∆Q where ∆Q represents the window of applicable momenta, In the case of this Gaussian, the purity of the reduced density is given by where √ N = Tr ρ red = ∆Q d 3 p 1 d 3 p 2 e − ( p 1 − p 2 ) 2 2σ 2 and the upper limit on the integrals means ∆Q d 3 p = ∆Q −∆Q dp x ∆Q −∆Q dp y ∆Q −∆Q dp z .
For small values of the dimensionless variance, σ 2 (∆Q) 2 < 1 , one then obtains The Rényi entropy (H 2 ) = − ln(Tr ρ 2 red ) is then given by Here, it should be understood that this expression has to be normalized in the limiting case σ 2 ≪ (∆Q) 2 . We circumvent the issue of normalization in the main text by using the linear entropy to quantify the entanglement of the pairs. But what is clear is that small values of the dimensionless variance lead to small deviations from the maximum entanglement.
If, on the other hand, the width σ is large and extends over all of the allowed range of momenta, then the state becomes effectively a product state as in Eq. (14) with uniform f 1 , f 2 . In this case, H 2 is small. This outcome is already clear by taking the limit of σ 2 /(∆Q) 2 → 1 in Eq. (18), as then Tr ρ 2 red → 1 so that H 2 → 0 .