## JHEP03(2017)013

Published for SISSA by Springer

Received: November 8, 2016 Revised: January 24, 2017 Accepted: February 9, 2017 Published: March 3, 2017

### On horizonless temperature with an accelerating mirror

Michael R.R. Good,^{a} Khalykbek Yelshibekov^{a} and Yen Chin Ong^{b,c}

aDepartment of Physics, School of Science and Technology, Nazarbayev University, 53 Kabanbay Batyr Ave., Astana, 010000 Republic of Kazakhstan

bCenter for Astronomy and Astrophysics, Department of Physics and Astronomy,
Shanghai Jiao Tong University, Shanghai, 200240 China^{1}

cNordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, Stockholm, SE-106 91 Sweden

E-mail: michael.good@nu.edu.kz,khalykbek.yelshibekov@nu.edu.kz, ongyenchin@sjtu.edu.cn

Abstract: A new solution of a unitary moving mirror is found to produce finite energy and emit thermal radiation despite the absence of an acceleration horizon. In the limit that the mirror approaches the speed of light, the model corresponds to a black hole formed from the collapse of a null shell. For speeds less than light, the black hole correspondence, if it exists, is that of a remnant.

Keywords: Black Holes, Field Theories in Lower Dimensions ArXiv ePrint: 1611.00809

1Present address.

## JHEP03(2017)013

Contents

1 Introduction: some puzzles with moving mirrors and evaporating black

holes 1

2 The machinery of moving mirrors 7

2.1 Some conventions of moving mirrors 7

2.1.1 The four functions of mirror physics 9

2.2 How to remove a horizon 10

3 The Domex trajectory 12

4 The energy production of Domex 12

4.1 The energy flux 12

4.2 Temperature of Domex 14

4.3 Total energy produced by Domex 15

4.3.1 Right side 16

4.3.2 Left side 16

4.3.3 Both sides 16

5 The entropy of Domex 17

6 The correlations in the radiation 19

6.1 Correlation functions 19

6.2 Correlation solutions 21

7 The particle production of Domex 21

7.1 The beta Bogoliubov coefficient integrals 21

7.2 Global particle distribution 23

7.3 Consistency check 24

8 Discussions 25

1 Introduction: some puzzles with moving mirrors and evaporating black holes

The discovery of Hawking radiation from a black hole came at a surprise over 40 years ago [1], since it implies that given enough time, black holes in asymptotically flat space- times would radiate off their mass; and if no new physics comes into play, they would eventually evaporate completely. This leads to the information paradox [2] — where did the information that falls into a black hole disappear to, if the black hole disappears com- pletely? Attempts to recover information from evaporating black holes continue to produce

## JHEP03(2017)013

new paradoxes, such as the firewall controversy [3–5], which threatens the conventional un- derstanding that there should be nothing unusual — much less a diverging energy density

— at the low curvature spacetime region near the event horizon of a sufficiently massive
black hole. In fact, the situation is worse than previously thought: if a firewall does ex-
ist, then in principle it can be much further away from the event horizon [6], so that an
unexpected space traveler would hit it and be burned to death even if he is nowhere near
a black hole. While the resolution of the information paradox may require us to fully un-
derstand how to unify general relativity with quantum field theory, it is certainly possible
that progress can nevertheless be made without a working theory of quantum gravity.^{1}
In recent years, it has become increasingly clear that we at least need to understand the
subtle “physics of information” [8–10], and how it applies to black holes [11–17], in order
to understand the information retrieval process from Hawking quanta.

In fact, a central piece of the puzzle regarding information loss, is the understanding of entanglement entropy,S. Let us consider the formation of a black hole from a gravitational collapse of some matter in a pure state. It is often believed that the entanglement entropy of the Hawking radiation received at null infinity, which should be zero at the beginning before any radiation arrives, should first increase, but then decrease at some point (known as the “Page time”), so that eventually the entanglement entropy vanishes. Such a “Page curve” [18–20] — the plot of the entanglement entropy against time — is crucial, since it gives insight into how information may be retrieved from the highly scrambled Hawking emission. There are, however, subtleties that are often overlooked. Notably, any calculation of entanglement entropy necessitates regularizing ultraviolet divergences. One notices that imposing a cutoff is a tricky procedure since modes that have sufficiently high energy at some point in the spacetime can be redshifted at some other point due to spacetime curvature. This implies that a mode that is beyond a cutoff scale can be red-shifted below the scale, so the cutoff is not well-defined [21,22]. Furthermore, the results obtained could depend on the cutoff scheme. Progress has been made recently with the introduction of the “causal-splitting regularization” scheme of Bianchi and Smerlak [23–25], which allows one to compute the production of entanglement entropy in a cutoff-independent manner.

However, even then, there are still a few puzzles regarding the entanglement entropy of an evaporating black hole. We list two such puzzles below.

(1) Negative Energy Flux and Negative Entropy: firstly, it has been observed, e.g. by
Bianchi and Smerlak [23,24], that mass loss of a black hole, assuming unitarity, is not
monotonic. In other words, at some point in time, the mass of an “evaporating” black
hole actually increases. For an observer at infinity, Hawking radiation reduces the
mass of a black hole by emitting particles. This means that an asymptotic observer
sees a flux of positive energy coming out from the black hole. If the mass increases,
albeit briefly,^{2} during the course of Hawking evaporation, this would correspond to
the emission of negative energy flux (hereinafter, “NEF”) from the black hole. (NEF

1Though we should probably first agree on what counts as a resolution of the paradox. See [7].

2Abdolrahimi and Page have also shown that for asymptotically flat Schwarzschild black holes, this increase in the mass is barely noticeable [26].

## JHEP03(2017)013

emission from evaporating black holes, at least in the case of a (1+1)-dimensional dilaton gravity, was already known in the literature for over 20 years [27].) Curiously, an observer equipped only with a particle detector would not be able to see any sign in the spectrum of the Hawking quanta to know that NEF has been emitted [28]. Even more surprising than the emission of NEF, in several models of evaporating black holes, Bianchi and Smerlak have explicitly shown that the entanglement entropy obtained from their causal-splitting scheme can also become negative at late times in the course of the evaporation. The physical interpretation of negative entropy is dependent on the particular type of entropy. Their physical relationships are subtle and not fully clear: in the literature it has been interpreted as either the radiation being less correlated than the vacuum [25], or the radiation being more correlated than the vacuum [29].

(2) Unitarity and Information Recovery: secondly, even with the fully covariant cutoff-
independent regularization of Bianchi and Smerlak, it was shown that [28] their crite-
rion only requires that the entanglement entropy tends to a constant asymptotically
(both in the far past and in the late future), instead of a more stringent requirement
that the entropy should tend to zero so as to recover the pure state. In fact, it is
not so surprising that the entanglement entropy can increase monotonically. Even
with the causal-splitting regularization, as long as there is a cutoff, then modes can
be redshifted by spacetime curvature, and consequently a mode that is below the
cutoff scale at future null infinity at some late time u, when traced back to the past
null infinity, could be well-above the cutoff. Since there is no longer a one-to-one
map between early modes and late time modes, it is not surprising that one does
not obtain S(u) →0 at late times. Note that such a phenomenon can be shown to
occur even in a simplified model involving a moving mirror in flat spacetime — as
was explicitly shown in [22, 28] — in which the quantum field theory is unitary. It
was suggested in [28] that the corresponding black hole picture might be a black hole
remnant [30,31], and that unitarity is maintained in the sense that if one takes into
account both the exterior and the interior of a black hole, then the entire quantum
state is pure at all times. In such a picture, information remains hidden inside the
ever-shrinking black hole horizon (the interior spacetime can still have a large vol-
ume [21,31–36], see however [37]) and the radiation is never purified. Since the end
state is a remnant, the information inside is never destroyed.^{3} It would be interesting
to investigate if S(u) → const. 6= 0 at late times necessarily implies that the cor-
responding black hole model ends as a remnant. A main question here, however, is
the following: do we understand entanglement entropy enough to base the debate of
information loss paradox of black holes on it? The subtleties here suggest that we
should be more careful in dealing with this issue.

3Note that there are two types of black hole remnant in the literature: the “long-lived” or “meta-stable”

remnant, and the “eternal” remnant [31]. The former has lifetime much longer than that of a black hole,
that is, proportional toM^{n}wheren >3. An eternal remnant, on the other hand, lives forever. Our model
corresponds to an eternal red-shifted scenario.

## JHEP03(2017)013

While Hawking evaporation has been a mainstay of the “quantum fields under exter-
nal conditions” enterprise, the moving mirror model [38, 39] has flourished mostly as an
ancillary effect. However, we feel that it is prudent to first understand a moving mirror
model in which both issues (1) and (2) can be investigated, after all, a (1+1)-dimensional
flat spacetime with a mirror trajectory is much simpler than a (3+1)-dimensional black
hole spacetime with non-trivial curvature.^{4} A trajectory of a moving mirror in spacetime
is a reflecting boundary on which field modes are constrained. A moving mirror excites the
modes, thereby producing particles. The spectrum of the emission depends on the exact
trajectory of the mirror. With a suitably chosen trajectory, we can therefore mimic the
particle production from, say, a collapsing star. (Readers who are not familiar with moving
mirrors can refer to [40] for a pedagogical exposition.)

Despite many decades of research, physical interpretations of external-potential type problems, like the moving mirrors, have never been made entirely clear. Moreover, serious confrontations with questions that are evaded in these non-gravitational analogs become inevitable during the study of gravitational problems. In other words, we would like to emphasize that one should not hope that a moving mirror model can fully resolve informa- tion paradox of a bona fide black hole, but understanding the subtleties of quantum field theory in a moving mirror model is a first step toward the more complicated physics of black holes.

We have come a long way in the study of moving mirrors. Notably, Moore [41], De- Witt [42], and later on, Davies and Fulling [38,39] initiated a program using field theories with external conditions, which eventually demonstrated that quantities like the expecta- tion values of the stress-energy tensor, and the localization of particles using wave packets, can be calculated in various physical problems and used to extract significant physical con- sequences of the quantum fields. Indeed, there has been renewed interest [23,24,43–54] in the moving mirror model in recent years due, in part, to claims of experimental verification of the dynamical Casimir effect [55, 56]. In many of these particle production scenarios, various systems that exploit the simple mathematical set up of the (1+1)-dimensional mov- ing mirror model have led to novel experimental designs. (See [54] for one of the latest proposals.)

As previously mentioned, a central advantage to the moving mirror model is its sim- plicity. This is both in general, and in the context of the recent one-to-one correspondence with a black hole [57–60], which found that for one concrete example, the particle produc- tion is exactly the same in both the mirror and black hole cases in (1+1)-dimensions. The simplicity of (1+1)-dimensions allows the crux of Hawking radiation to stand out more clearly, separated from the specialized details associated with higher dimensional curved geometry and back-scattering. With the one-to-one correspondence, the moving mirror model can be treated as an even more precise analogy to Hawking’s original argument, and therefore it is of interest to extend the one-to-one correspondence to more physically

4Einstein’s gravity is topological in (1+1)-dimensions, but with a suitable coupling to matter fields, gravity need not be trivial in (1+1)-dimensions. This allows one to study black hole evaporation. In our moving mirror model, of course, there is no gravity, only an accelerating mirror, so there is no complication either.

## JHEP03(2017)013

realistic circumstances, while holding on to this fortunate simplicity. However, even as
a relatively simple theoretical model of black hole evaporation in (1+1)-dimensions, the
moving mirror model, has in practice, been very hard to extend to solutions for exact tra-
jectories where the global Bogoliubov coefficients may be evaluated. Few solutions have
been found^{5} and finite-nonzero-energy cases are scarce.^{6} Nevertheless, mirror trajectories
that produce finite amount of energy are precisely those that are physically more realistic.

We are therefore interested in such trajectories.

Although there is pedagogical value associated with the reduced complexity of the
direct and straightforward calculations in the moving mirror model in (1+1)-dimensions,
one should note that there is a peculiarity in (1+1)-dimensions, namely that Minkowski
spacetime in (1+1)-dimensions have two sets of past and future null infinities. The right
past infinity will be denoted by I_{R}^{−}, and the right future infinityI_{R}^{+}. Similarly, we also
have I_{L}^{−} and I_{L}^{+}. That is to say, its Penrose diagram is a diamond, whereas in higher
dimensions, the Penrose diagram for Minkowski spacetime is a triangle.^{7} The implication
is this: if we want to understand quantum field theory of a moving mirror in (1+1)-
dimensions, we should also take into accountthe left side of the mirror.

Yet another motivation to consider both sides of the mirror is the following: in (1+1)-
dimensional conformal field theory, there are left and right “temperatures”, T_{L} and T_{R},
which are related to the amount of left and right-moving excitations in the field. In a
thermal ensemble of states, the thermodynamic temperature is related to these left and
right temperatures. The Cardy formula for microstate degeneracy [65],

S_{micro} = π^{2}

3 (c_{L}T_{L}+c_{R}T_{R}), (1.1)

explicitly involves these temperatures, along with the left and right central charges cL and
c_{R}. So from this point of view of thermodynamics, it is natural to include both left and
right-moving excitations.

The most important reason to consider both sides of the mirror, however, is related to the eventual aim to understand information loss of black holes. To do so, as we have argued, a crucial first step is to understand how entanglement works in the simpler case of a moving mirror. In particular, as far as unitarity is concerned, it is important that we include the entire spacetime, this is to ensure that information is not hiding in some part of spacetime that one might otherwise overlook.

In this work, we are mainly motivated in asking the following questions:

Is there a moving mirror in (1+1)-dimensions, satisfying unitarity in the sense allowed by the Bianchi-Smerlak criterion (namely,S(u)→const. asu→ ±∞),

5For example: the case of uniform acceleration of Davies-Fulling [39]; and the case of eternal thermal emission of Carlitz-Willey [61].

6See the first known solution found by Walker-Davies [62] and the asymptotically static case in Good- Anderson-Evans [63] and a drifting case in Good-Ong [28].

7It is true that one often draws the Penrose diagram of Minkowski spacetime as a diamond even in higher
dimensions, but the point is that in (2+1)-dimensions and above, the two points that represent spacelike
infinityi^{0}, are actuallyone and the same. This is clearer if one looks at how the conformal diagram wraps
around the Einstein cylinder (see figure 14 on page 122 of [64]). In (1+1)-dimensions, the two points are
genuinely different infinities.

## JHEP03(2017)013

that has no acceleration horizon, produces finite amount of energy, and serves as an analog for Eddington-Finkelstein coordinate null-shell gravitational collapse in its limiting case? Furthermore, by looking at both sides of the mirror trajec- tory, can we understand, or at least reveal some additional features, regarding negative energy flux and negative entropy?

We shall now explain the reason we would like to consider only trajectories that have no acceleration horizon (hereinafter, we will simply refer to an acceleration horizon as

“horizon”, unless there is a risk of confusion). The basic utility of various trajectories ex- amined in the moving mirror model with respect to black hole radiation has, like black hole evaporation itself, also been well-known for over forty years. But the problem of relating Hawking’s global construction calculation (see [66] for a stochastic route) to the physical mechanism responsible for the particle-energy creation effect, which is safely assumed to involve local curvature, has been mostly elucidated by various methods using thelate-time Davies-Fulling black hole-moving mirror correspondence. However, with the advent of the all-time, exact, black hole-moving mirror correspondence [57], the physics of the boundary condition effect is more directly related to the curved space effect than previously sup- posed. We therefore hope to timely exploit this insight by extending the flat-space model to one with a boundary condition that doesnot contain an asymptotic horizon. It is clear from basic causality that the existence of a horizon in the future is not essential to the production of particles and energy at early times, and in this calculation we will explicitly demonstrate the particle production by localization of the spectra at early times. (In fact, the same causality argument works for the case of a black hole, i.e. the event horizon is not an essential feature for early-time particle creation. See also [67].)

Beyond this, we will demonstrate thatthe production process at any time need not have an acceleration horizon in order to reach thermal equilibrium. The use of wave packets to obtain spectral resolution of thermal Hawking radiation in such a limiting-case horizonless model where the evaporation process stops at late times, has not been investigated before.

It is important to recognize that this model is an extension of the particular moving mirror which has a one-to-one correspondence to the exactly solvable black hole case [57]. The model presented here is novel, in part, because its limit is that of the exact correspondence, which means that a certain acceleration parameter (see below) is appropriately scaled. A novel result of the removal of the horizon, for this unique trajectory, is that the finite total emission of energy is simple enough that it can be expressed analytically. Also important to this solution is the introduction of a new method to find other moving mirror solutions which may otherwise be intractable.

In this work, we are focused on the mirror model. Although the solutions and their novel features could represent various black hole collapse scenarios, it is premature to make any strong conclusion here. In addition, even though the moving mirrors that we investigate below have no acceleration horizon, this does not necessary mean that the corresponding

“black holes” have no event horizon^{8}(or at least a trapped surface of some sort). After all,

8The possibility that black holes may not have an event horizon has been investigated by many authors, see [68,69] and the references therein.

## JHEP03(2017)013

a main purpose of moving mirror models is to reproduce particle emission of a black hole

— it is the properties of the produced particles that are in correspondence — one should
be very careful if one wishes to identify the mirror trajectories themselves to geometric
properties of black holes such as the event horizons.^{9}

The present work is organized in the following manner. A short introductory treatment
of the moving mirror machinery is given in section2. It shows how to generalize the exactly
solvable “black mirror” case to remove the horizon. The subject of interest in section 3
is the explicit trajectory of our new mirror solution. In section 4 we solve for the energy
flux and the total energy production on both sides of the mirror. The energy flux is shown
to have a spike on the left side and a plateau on the right side. We also quantify the
equilibrium temperature. In section 5 we calculate the entanglement entropy flux and
confirm it remains consistent with the energy-entropy relation and unitarity. In section 6
we investigate the stress tensor correlations for the model by solving for the correlation
ratio R_{1} exactly. This helps confirm thermal equilibrium. In section 7 we calculate the
particle production and investigate the spectral dynamics. Here we include consistency
checks to verify the total energy produced via the stress tensor, agrees with the total energy
produced from summing particle quanta. We find constant emission of particles emitted
to the observer on the right for any arbitrary long period of time. We conclude with some
discussions in section 8. Throughout this work, we use the units G=c=~=k_{B}= 1.

2 The machinery of moving mirrors

In section2.1, we shall first introduce some basic concepts necessary for understanding our construction of a horizonless solution that generalizes the “black mirror”. We then discuss the removal of the acceleration horizon in section2.2. The solution satisfies three criteria:

the presence of a horizonless temperature, an appropriately scaled acceleration parameter, and the termination of evaporation at late times.

2.1 Some conventions of moving mirrors

As the simplest example of the dynamical Casimir effect, the moving mirror model also
serves as a way to understand black hole evaporation by imposing an external bound-
ary condition in 1+1 dimensions on the quantum field, rather than an external curved
spacetime. Consider then, such a boundary that does not accelerate forever, starting and
ending at time-like past infinityi^{−}, and time-like future infinityi^{+}, respectively; possessing
asymptotically zero acceleration in both the far past and far future, and always moving
slower than the speed of light. This fully asymptotically inertial mirror will contain no
horizon. Thus, it will contain no pathological acceleration singularity either. The plot of
such a trajectory is in figure 1. A salient pay-off for horizon-removal is that the mirror
system, in addition to being unitary (henceforth, by unitarity we always mean unitarity

9While it is true that an accelerated observer in Rindler spacetime sees Unruh temperature that is analogous to the Hawking temperature of a black hole, it does not follow that an acceleration horizon of a mirror always corresponds to a black hole horizon. Furthermore, the temperature in the mirror case, is measured by observers far away from the mirror, not a Rindler-like observeronthe mirror trajectory.

## JHEP03(2017)013

I L

**+** I

R
**+**

I L

**-** I

R
**-**

i^{0}
i^{0}

i^{+}

i^{-}

t

x

Figure 1. Left: in this Penrose diagram, the color curves are “Domex”, with asymptotically inertial trajectories. The black curve is “Omex”, a horizon mirror (moving mirror with a horizon) [57]. The different coasting speeds correspond toξ= 0.6,0.7,0.8,0.9, for green, blue, red, purple, respectively.

Right: the asymptotically inertial trajectories (Domex) with the same final coasting speeds displayed
in the usual spacetime diagram. The dashed lines represent the light cone, and the dotted-dashed
horizon line is at v_{H} = 0. The trajectory example here is the same as in the conformal diagram.

For comparison, the black line indicates the horizon mirror (Omex) [57], which contains a horizon coinciding with the light cone.

in the broad sense allowed by Bianchi-Smerlak criteria), produces only a finite amount of total energy, as we will demonstrate in section 4 and section5.

The quantum field, Ψ, is the massless scalar of the Klein-Gordon equation Ψ = 0,
whose value is zero, Ψ|_{z} = 0, when evaluated at the position of the moving mirror, z(t).

The modes, φω^{0} and ψω, are on equal footing in the sense that they can both be used to
expand the field:

Ψ = Z ∞

0

dω^{0}
h

a_{ω}^{0}φ_{ω}^{0}+a^{†}_{ω}0φ^{∗}_{ω}^{0}
i

= Z ∞

0

dω h

bωψω+b^{†}_{ω}ψ^{∗}_{ω}
i

. (2.1)

The modes are orthonormal and complete and can be exactly solved in the (1+1)-dimen- sional case:

φ_{ω}^{0} = (4πω^{0})^{−1/2}[e^{−iω}^{0}^{v}−e^{−iω}^{0}^{p(u)}], (2.2)
ψω = (4πω)^{−1/2}[e^{−iωf(v)}−e^{−iωu}], (2.3)
where the functionsp(u) andf(v) are the usual notation for the ray-tracing functions, which
are intimately related to the trajectory of the mirror z(t) itself, see [63] and section 2.1.1.

The famous Bogoliubov coefficients appear by expanding one set of modes in terms of the

## JHEP03(2017)013

other set of modes,

φ_{ω}^{0} =
Z ∞

0

dω [α_{ω}^{0}_{ω}ψ_{ω}+β_{ω}^{0}_{ω}ψ^{∗}_{ω}], (2.4)
ψ_{ω}=

Z ∞ 0

dω^{0} [α^{∗}_{ω}0ωφ_{ω}^{0}−β_{ω}^{0}_{ω}φ^{∗}_{ω}0], (2.5)
where

αω^{0}ω = (φω^{0}, ψω), βω^{0}ω =−(φ_{ω}^{0}, ψ^{∗}_{ω}), (2.6)
with the flat space scalar product defined in null coordinates, (u, v), by

(φ_{ω}^{0}, ψω)≡i
Z ∞

−∞

du φ^{∗}_{ω}^{0}

↔

∂uψω+i Z ∞

−∞

dv φ^{∗}_{ω}^{0}

↔

∂v ψω. (2.7)

The Bogoliubov coefficients α_{ω}^{0}_{ω} and β_{ω}^{0}_{ω} also give the operators a_{ω}^{0} and a^{†}_{ω}0 in terms of
the operatorsb_{ω}andb^{†}_{ω}, while the orthonormality of the modes hold according to the usual
convention, see [28] for more detail.

2.1.1 The four functions of mirror physics

There are four functions,vs(u),us(v),xs(t),ts(x), which are useful for doing global calcula- tions involving the aforementioned field modes. The first two are the ray-tracing functions (expressed in null coordinates), where us(u)≡p(u) andvs(v)≡f(v), and the last two are the associated spacetime coordinate functions. The inverses are expressed like so:

us(v) =v_{s}^{−1}(u), xs(t) =t^{−1}_{s} (x). (2.8)
We shall collectively call all four of them, “shock wave functions” or “shock functions”

for short, after the collapse of the null shell shock wavefront description to form a black
hole. There are many other auxiliary functions, such as t_{s}(v),v_{s}(t),t_{s}(u), u_{s}(t). However,
the original four functions of coordinates v, u, t, and x will prove efficient at calculating
observables. The information about how the field modes become red-shifted due to external
conditions is fully contained in these four functions. The relationships between them are
demonstrated as follows.

First consider the usual null coordinates on Minkowski spacetime u ≡t−x and v ≡ t+x, and their analogous auxiliary functions as functions of time,

u_{s}(t) =t−x_{s}(t), v_{s}(t) =t+x_{s}(t). (2.9)
These contain the shock functionxs(t), which is the trajectory of the mirror. The inverses
of eqs. (2.9), contain the shock functions, u_{s}(v) andv_{s}(u),

ts(u) = 1

2(vs(u) +u), ts(v) = 1

2(us(v) +v). (2.10) Functional inverses should be obvious from the notation. Useful auxiliary inverses are:

ts(u) = u^{−1}_{s} (t), and ts(v) = v_{s}^{−1}(t). The total energy emitted, the energy flux, and the
beta Bogoliubov coefficients have expressions that are conveniently written in terms of the
four shock functions.

## JHEP03(2017)013

2.2 How to remove a horizon

There is an easy way to remove the horizon, (recall that c= 1),

t→+∞lim |˙z(t)|= 1, (2.11)

from a future asymptotically null moving mirror trajectory, z(t). The idea is to modify this so that the new trajectory, z(t), has

t→+∞lim |z(t)|˙ =ξ, (2.12) where 0 < ξ < 1 is the future asymptotically drifting speed. This can be achieved by writing the horizonless trajectory,z(t), in terms of the trajectory with a horizon (henceforth

‘horizon trajectory’), z(t),

z(t) =ξz(t). (2.13)

This works if

˙

z(t) =ξz(t).˙ (2.14)

Taking this approach helps answer whether the particle spectra can (1) reach equilibrium for an extended period of time, and (2) proceed to shut off. The mirror does not strictly have a null horizon, yet as we will see, it can still achieve a “thermal plateau” (i.e. the emission is virtually thermal for some arbitrary finite amount of time). This approach also ensures (3) the correct scale for the acceleration parameter κ (not to be confused with the physical acceleration, see below). A correct scale is critical for the red-shifting of the modes to correspond to the exactly solvable black hole case [57–60] in the limit ξ → 1.

This automatically extends the mirror in the black hole-moving mirror correspondence by promoting it to a more physical footing where the total evaporation energy is finite and unitarity is preserved.

While we have found the mirror solution that meets these strict requirements, a possible
black hole counterpart calculation is beyond the scope of this work. In the model we are
about to present, we do not claim that it actually corresponds to any realistic evaporating
black hole spacetime. For the present work we only seek a simple mirror model in which
the three conditions presented above are met, so that we may study the energy and energy
flux, the entropy, the correlations, and the particle spectra, together in the absence of a
horizon. It may or may not have an exactly tractable black hole correspondence. In a
subsequent work this will be investigated, but as we have emphasized in the Introduction,
even if it has such a black hole correspondence, the absence of horizon in the mirror model
does not necessary entail the absence of any event horizon or trapped surface in the black
hole geometry. It is worth pointing out that this mirror solution is new — it is the first
explicit demonstration of a unitary solution with a thermal plateau^{10} that has limiting
red-shifting functions which correspond to the black hole-moving mirror system in [57].

10Other unitary plateau investigations exist, see section8for a discussion of one.

## JHEP03(2017)013

The information contained in the trajectory equation of motion of the mirror is also contained in the shock functions. The exactly solvable mirror case in [57] has shock func- tions:

vs(u) = v_{H}−κ^{−1}W
h

e^{κ(v}^{H}^{−u)}
i

, (2.15)

u_{s}(v) = v−κ^{−1}ln [κ(v_{H}−v)], (2.16)
xs(t) = vH−t−(2κ)^{−1}W

h

2e^{2κ(v}^{H}^{−t)}
i

, (2.17)

ts(x) = vH−x−κ^{−1}e^{x/2κ}. (2.18)

The W is the product log or W Lambert function, which commonly appears in thermal
equilibrium contexts, e.g. Wien’s law.^{11} One way to get these is as follows: firstly, one
has the simple formu_{s}(v) as it is a simple choice for redshifting ray-tracing f(v) function
in the mirror case (or from the spacetime matching solution in the null-shell case). This
is given. Secondly, one takes the inverse to get vs(u). While easy, as it turns out, it was
unhelpful in obtaining the other shock wave functions. The efficient approach is to notice
thatus(v) has a simpler form thanvs(u), so one usesus(v) again to write downts(v). The
inverse of this can be calculated. It is, of course, vs(t). (Note that if one choosesvs(u) to
write downt_{s}(u) instead, the inverse is not quite as straight-forward to compute, in fact it
is much more complicated.) So, usingvs(t), one is set to write down xs(t) =vs(t)−t. Its
inverse is, fortuitously tractable, and gives the above expression for t_{s}(x).

We shall interchangeably call the horizon trajectory in the mirror analog case the “black
mirror” [60] or “Omex” for short [57]. (“Om”-after the Omega constant,W(1) = Ω = 0.567
where Ωe^{Ω} = 1, and ‘ex’ after the exponent in W argument.) The acceleration parameter
κ in the black mirror case can be identified with the surface gravity in the black hole case,
κ= (4M)^{−1}, for all times.

The new moving mirror has the following more complicated shock functions:

vs(u) = 2ξ

1 +ξvH+1−ξ 1 +ξu− ξ

κW

2e

2κ(vH−u) 1+ξ

1 +ξ

, (2.19)

u_{s}(v) =− 2ξ

1−ξv_{H}+1 +ξ
1−ξv+ ξ

κW

2e

2κ(vH−v) 1−ξ

1−ξ

, (2.20)

xs(t) =ξ vH−t−W

2e^{2κ(v}^{H}^{−t)}
2κ

!

, (2.21)

t_{s}(x) =v_{H}− x
ξ − 1

κe^{2κx/ξ}. (2.22)

While these expressions still depend on the primary parameter κ, the intricacy of these
expressions arises from the introduction of a second parameter, ξ. Recall that v_{H} in the
black mirror case is the location of the horizon. We retain vHfor completeness, but make
no mistake: the mirror no longer asymptotes to infinite acceleration at a null horizon,

11The maximum frequency of the (3+1)-dimensional Planck distribution, _{π}^{V}_{2}_{c}^{~}_{3} ^{ω}^{3}

e^{β~ω}−1, isβ~ωmax = 3 +
W

−_{e}^{3}3

, i.e. the famous displacement lawβ~ωmax= 2.82144.

## JHEP03(2017)013

located atv_{H}. We shall therefore refer tov_{H}as a “residual horizon”. This mirror begins at
rest in the far past, and therefore has no initial asymptotic horizon either. The absence of
horizons generates the finite total energy, akin to the notion that evaporating black holes
exhale only a finite energy flux [70–73].

3 The Domex trajectory

The motion of the mirror is given by the trajectory eq. (2.21), z(t) =−ξ

1 2κW

2e^{−2κt}
+t

, (3.1)

wherevH= 0 for simplicity, and 0< ξ <1 is the final speed of the mirror as t→ ∞. The motion is initially asymptotically static, limt→−∞z(t) = 0, and most notably, the mirror˙ does not approach a future asymptotically static resting state because its future asymptotic speed is

t→+∞lim |z(t)|˙ =ξ, (3.2)

making this trajectory future asymptotically coasting. The future drifting feature of this mirror means it is an exact model for a remnant [28, 30, 31] as described by an early anticipation of such solutions by Wilczek in [74].

The trajectory eq. (3.1) is plotted in both the spacetime and Penrose diagrams in
figure1. The acceleration parameter, κ, isκ >0, and to be clear, it isnot the acceleration
of the mirror,α(t)6=κ. The rectilinear proper acceleration, α=γ^{3}z, is time-dependent:¨

α(t) =− 2κξW 2e^{−2κt}
(W(2e^{−2κt}) + 1)^{3}

1− ^{ξ}^{2}

(W(2e^{−2κt})+1)^{2}

3/2. (3.3)

The negative sign on eq. (3.3) gives a mirror whose motion is to the left. The acceleration has asymptotic behavior such that

t→±∞lim α(t) = 0, (3.4)

making this trajectory asymptotically inertial, despite the drift. As we shall now show, this solution has several analytically tractable results. The special physical aspects of this solution will be investigated in the following sections. We shall refer to this horizonless mirror as Drifting-Omex (“Domex”) for short.

4 The energy production of Domex

4.1 The energy flux

The energy flux of a moving mirror was first derived by Davies and Fulling [38]. Expressed in terms of the shock functions, it may be computed via

F(u) = 1 24π

"

3 2

v^{00}_{s}
v_{s}^{0}

2

− v_{s}^{000}
v_{s}^{0}

#

, (4.1)

F(v) = −1 24π

"

3 2

u^{00}_{s}
u^{0}_{s}

2

−u^{000}_{s}
u^{0}_{s}

# 1

u^{02}_{s} , (4.2)

## JHEP03(2017)013

-10 -5 5 10

### t

20 40 60

### F

-10 -5 5 10

### t

-0.4 -0.2 0.2 0.4 0.6 0.8 1.0

### F

Figure 2. Left: the left observer sees energy flux that strongly peaks the faster the coasting speed
of the mirror: ξ = 0.6,0.7,0.8,0.9, colored by green, blue, red, purple, respectively. Notice the
initial NEF, and the above-thermal, F(t)>1, emission. Hereκ^{2}= 48π. Right: successive plots of
the energy flux observed by the right observer, F(t)≡ hT_{uu}i, eq. (4.6), from smallest peak to the
largest peak, with varying limiting mirror speeds,ξ= 0.6,0.7,0.8,0.9. Also included areξ= 1−0.1^{x}
wherex= 2,3,4,6 colored by orange, pink, cyan, black, respectively. Thermal equilibrium occurs
only for a very fast final coasting speed. The total NEF is qualitatively unchanged at this speed.

The acceleration parameter is set to κ^{2} = 48π so that the plateau levels out at F = 1, the dot-
dashed line.

F(t) = 1 12π

x^{000}_{s}(x^{02}_{s} −1)−3x^{0}_{s}x^{002}_{s}
(x^{0}_{s}−1)^{4}(x^{0}_{s}+ 1)^{2}

, (4.3)

F(x) = 1 12π

t^{000}_{s}(t^{02}_{s} −1)−3t^{0}_{s}t^{002}_{s}
(t^{0}_{s}−1)^{4}(t^{0}_{s}+ 1)^{2}

. (4.4)

In terms of a u-dependent rapidity [57],η(u)≡tanh^{−1}[z(t˙_{u})] = ^{1}_{2}lnv_{s}^{0}(u), this is
F(u) = 1

12π η^{02}−η^{00}

. (4.5)

Right side. The energy flux, emitted to an observer at the right side of the mirror,I_{R}^{+},
using the trajectory of eq. (3.1) in eq. (4.3), is therefore easily calculated:

F(t) =

κ^{2}ξW 2e^{−2κt}

ξ^{2}+ 2W 2e^{−2κt}2

+W 2e^{−2κt}

−1

3π(−ξ+W(2e^{−2κt}) + 1)^{2}(ξ+W (2e^{−2κt}) + 1)^{4} . (4.6)
It contains a build-up phase, a thermal plateau, and an end-phase accompanied by negative
energy flux (NEF), see figure2. The residual horizon location has been set tov_{H}= 0.

A period of thermal emission occurs at extremely high coasting speeds, giving a thermal plateau, which is, in the limit ξ→1, located for some time ∆tT P, at

F(∆t_{T P})≈F_{T} ≡ κ^{2}

48π. (4.7)

Interestingly, this is the same as the constant flux produced by the (eternally thermal) Carlitz-Willey trajectory [61]. The Carlitz-Willey mirror radiates a thermal Planckian

## JHEP03(2017)013

distribution of particles for all times, at F =F_{T}. In our model, this value occurs because
in the limit ξ → 1, this mirror has the same shock functions as the black mirror, which
has thermal radiation at late times. However, now it is apparent that in this model, the
evaporation eventually stops, effectively decoupling the late-time approximation from the
high-frequency approximation.

Allowing ξ to be nearly the speed of light, (for example, ξ = 1–0.1^{10}, with no formal
limit), the energy flux emitted to the right observer, has a simple minimal negative value,
at some late time, t0, where

F(t_{0})^{min} =−1

3F_{T}, (4.8)

which is a fairly significant proportion of the maximum magnitude amplitude of thermal emission.

Left side. The energy flux, emitted to an observer at the left of the mirror, I_{L}^{+}, using
the trajectory of eq. (3.1) by symmetry reversing the sign on ξ, is:

F(t) =−

κ^{2}ξW 2e^{−2κt}

ξ^{2}+ 2W 2e^{−2κt}2

+W 2e^{−2κt}

−1

3π(−ξ+W (2e^{−2κt}) + 1)^{4}(ξ+W(2e^{−2κt}) + 1)^{2} . (4.9)
The energy flux contains an initial nascent NEF, a rapid reversal to positive energy flux
and build-up to a non-thermal positive energy flux peak, and finally a rapid end-phase
that falls to zero emission, see figure 2. It is now clear that while one side of the mirror
is approaching thermal equilibrium emission, the other side is experiencing a single non-
thermal, ever-more-narrow burst, demonstrating a characteristic difference between the left
and right observers. We investigate the pulse via particle spectra in section 7.

4.2 Temperature of Domex

Domex achieves a temperature, 2πT =κ, to lowest order inwhereξ ≡1−, via a “twice
rapid acceleration” (κ(u) =|p^{00}/p^{0}|=|2η^{0}|) approximation. The rapid acceleration,η^{0}(u), is
identically constant, such that κ(u) =κ, for the eternally thermal mirror (Carlitz-Willey).

One finds,

2πT =|2η^{0}|=κ(1 +W(e^{−κu}))^{−2}+O(). (4.10)
For largeκu, so long as,κu≪^{−1}, thenW(e^{−κu})→0, and to lowest order in, the rapid
acceleration is constant, 2πT =|2η^{0}|=κ.

From the energy flux production, we can help quantify the equilibrium condition of
Domex. The simplicity of the time-space function, t_{s}(x), allows for analytic tractability.

Finding where the radiation is most near equilibrium amplitude, F ≈ FT ≡ κ^{2}/(48π) is
possible. Using v_{H} = 0, and ts(x) =−κ^{−1}e^{2κx/ξ} −x/ξ, one has the flux as a function of
space:

F(x, ξ, κ) =

2κ^{2}ξe^{2κx}^{ξ}

8e^{4κx}^{ξ} + 2e^{2κx}^{ξ} +ξ^{2}−1

3π

−2e^{2κx}^{ξ} +ξ−1
2

2e^{2κx}^{ξ} +ξ+ 1

4. (4.11)

## JHEP03(2017)013

Maximizing F(x, ξ, κ) with respect to x, gives the spatial location, x_{0}, where the flux is
maximum, F(x0, ξ, κ) = Fmax(ξ, κ). Since drift speed is high, then to lowest order in ,
ignoring the imaginary component of this spatial locus, the real location is

x0 = 1 6κln

6 +O(^{1/3}). (4.12)

The maximum flux, to lowest order in , is then
F(x_{0}, ξ, κ) =F_{max}(ξ, κ) = κ^{2}

48π

1−3√^{3}

6^{2/3}+25

3 +O(^{4/3})

. (4.13)

Following Davies [39], eq. (3.10), or Walker [75], eq. (5.10), we consider the property that the energy flux of a thermal trajectory has

F = Z ∞

0

dω 2π

ω

e^{ω/T} −1 = π

12T^{2}. (4.14)

Temperature can be expressed as,

T(ξ, κ) = r12

π Fmax(ξ, κ), (4.15)

where we have taken the positive root, T >0. To low order in, the result is T(ξ, κ) = κ

2π

"

1−3 3

4 1/3

^{2/3}+ 25

6 +O(^{4/3})

#

. (4.16)

The lowest order dependence on drift speed scales as ∼ (1−ξ)^{2/3}, indicating, e.g. that
speeds of ξ = 1–0.1^{9} give a millionth part deviation from equilibrium temperature. To
ensure Domex is very near equilibrium for an extended period of time, we will use speeds
far faster while investigating the time dependence of particle production in section 7.

4.3 Total energy produced by Domex

It proves possible to calculate the finite total emitted energy analytically. In terms of the shock wave functions, the total energy to the right side of the mirror, is computed via,

E = Z ∞

−∞

F(u) du, (4.17)

E = Z ∞

−∞

F(v)u^{0}_{s}dv, (4.18)

E = Z ∞

−∞

F(t)(1−x^{0}_{s}) dt, (4.19)

E = Z −∞

+∞

F(x)(t^{0}_{s}−1) dx, (4.20)

## JHEP03(2017)013

or after integration by parts, where the boundary term is ignored due to asymptotic inertial character,

E = 1 48π

Z ∞

−∞

v_{s}^{00}
v_{s}^{0}

2

du, (4.21)

E = 1 48π

Z ∞

−∞

u^{002}_{s}

u^{03}_{s} dv, (4.22)

E = 1 12π

Z ∞

−∞

x^{002}_{s}

(1 +x^{0}_{s})^{2}(1−x^{0}_{s})^{3} dt, (4.23)
E = 1

12π Z ∞

−∞

t^{002}_{s}

(1 +t^{0}_{s})^{2}(1−t^{0}_{s})^{3} dx , (4.24)
where vs ≡ vs(u), us ≡ us(v), xs ≡ xs(t) and ts ≡ ts(x). The primes always mean
derivatives with respect to the respective function variable. For the mirror trajectory
here with finite energy production we shall use the x_{s}(t) integral over dt and confirm it
with quanta summing of particles in section 7, where the total emitted energy is E =
R∞

0 dω ωR∞

0 dω^{0} |β_{ωω}^{0}|^{2}.

Note that by “total”, we mean that it is the total amount of energy that only the observer on the right side detects. The mirror emits energy on both sides to two separate observers: left and right. To find the energy emitted to the left, by symmetry, one can simply reverse the motion and compute the energy on the right side again.

4.3.1 Right side

The total energy radiated to I_{R}^{+} is therefore:

ER= κ(3−ξ) tanh^{−1}(ξ)

48πξ^{2} − κ(3 + 2ξ)

48π(ξ^{2}+ξ). (4.25)

Domex does not result in the emission of infinite energy to the usual observer atI_{R}^{+}. Note
that the solution here is monotonic for increasing coasting speed and never negative for
0< ξ <1. Here, the lim_{ξ→0}E_{R}= 0, and the lim_{ξ→1}E_{R}= +∞.

4.3.2 Left side

For an observer to the left atI_{L}^{+} the total energy emitted is found by simply substituting,
ξ→ −ξ, intoE_{R},

E_{L}= κ(3 +ξ) tanh^{−1}(−ξ)

48πξ^{2} − κ(3−2ξ)

48π(ξ^{2}−ξ). (4.26)

Again, the energy is finite as long as the speed is less than the speed of light. The expression,
E_{L}(ξ) is a monotonic function ofξ.

4.3.3 Both sides

For the high coasting speeds we are interested in, the energy emitted to the left is always
much greater than the energy emitted to the right, E_{L} E_{R}. For small values ofξ one
finds

EL

E_{R} = 1 + 6

5ξ+O(ξ^{2}), (4.27)

## JHEP03(2017)013

0.2 0.4 0.6 0.8 1.0

**ξ**

10^{-4}
0.01
1
100

### E

_{T}

**,**L

**,**R

0.2 0.4 0.6 0.8 1.0

**ξ**

0.5 1.0 1.5 2.0

### E

_{T}

**,**L

**,**R

Figure 3. Left: energies plotted in a semi-log plot. The total energy emitted is the black line,
ET(ξ) = _{24π}^{κ} _{1−ξ}^{1}2−^{tanh}_{ξ}^{−1}^{ξ}

, withκ= 24πin a log plot. The energy diverges as the final coasting
speed approaches the speed of light. The red line is the EL and the blue line isER. Right: the
same energies,E_{T},E_{L}, andE_{R}, plotted to scale,κ= 24π.

indicating that EL > ER. As it turns out, EL> ER for all values of the final drift speed,
0< ξ <1. The total energy emitted to both observers isE_{T} =E_{L}+E_{R}:

E_{T} = κ
24π

cosh^{2}(η)−ηcoth(η)

, (4.28)

whereη= tanh^{−1}ξ, is the final rapidity. See figure 3to see a graph of the combined total
emitted energy from both sides of the mirror. Notice the divergent behavior as the coasting
speed approaches the speed of light. The energy increases monotonically as a function of
the coasting speed.

5 The entropy of Domex

The von Neumann entanglement entropy in the unitary moving mirror case, can be found
from Bianchi-Smerlak’s formula^{12} [24] as a function ofvs(u)≡p(u),

S(u) =− 1

12lnp^{0}(u). (5.1)

In terms of the mirror trajectory (see Good-Ong [28]), this is S(t) =−1

6tanh^{−1}[ ˙z(t)] =−1

6η(t), (5.2)

where z(t) is the trajectory motion of the moving mirror, the dot represents the time
derivative and η(t)≡tanh^{−1}[ ˙z(t)] is the time-dependent rapidity. It is simple to see that

12Here the central charge for a conformal field theory,c, has been set to unity without loss of generality.

## JHEP03(2017)013

-4 -2 2 4 6 8 10

### t

-1.5 -1.0 -0.5

### S

_{L}

-4 -2 2 4 6 8 10

### t

0.5 1.0 1.5

### S

_{R}

Figure 4. The von Neumann entanglement entropy, for the left and right sides of the mirror respectively, as a function of time, withξvalues and colors as the previous figure2 but hereκ= 1.

The entropy approaches a constant value, underscoring the final asymptotic coasting speed of the mirror and the eventual end of particle emission, with no turn over of the Page curve. All left moving field modes become right moving field modes, and vice versa, preserving unitarity.

the faster the mirror moves, the greater the entropy. Unitarity in this sense strictly means that the entropy must achieve a constant value in the far past and far future. The mirror we consider has a non-zero asymptotic entropy, underscoring that eternally thermal radiation is not the end state. Since evolution from a possible initially pure state, to a final mixed state does not occur, radiation of energy flux stops and it is possible to reestablish a possible initial pure state, preserving unitarity. This mirror’s trajectory is found to be consistent with the Bianchi-Smerlak [24] entropy-energy relationship

2πF(u) = 6S^{0}(u)^{2}+S^{00}(u), (5.3)
where the entropy for Domex, expressed as a function of time, t, for both the right and
left sides,

S_{L}^{R}(t) =±1

6tanh^{−1} ξ

W 2e^{2κ(v}^{H}^{−t)}
+ 1

!

, (5.4)

approaches a constant value,

t→∞lim S_{L}^{R}(t) = 1

6tanh^{−1}(ξ) =±η

6, (5.5)

as the energy flux approaches zero. Notice the independence of κ or the position of the horizon vH for the final entropy value. Here η is the final coasting rapidity (ξ is the final coasting speed). These results are in dramatic contrast to Omex [57] which has infinite total energy and a divergent entanglement entropy in the far future, t →+∞. A plot of the entropy (on both sides of Domex), eq. (5.4), is in figure 4.

For Domex, the entanglement entropy has no turn-over of the Page curve [18–20] as it is monotonically increasingly approaching some constant value. Although outside the scope of this work, it is worth mentioning that the radiation in an analogous black hole context would never get purified. The preservation of unitarity is maintained only in the sense

## JHEP03(2017)013

that the pure state remains pure taking into account both the exterior and interior [30]

of the black hole remnant. There are unresolved challenges associated with this type of scenario stemming from the known infinite production problem, stability, and energy conservation. Detailed discussions are provided in [31]. Note however, that Domex, as a possible candidate model for a remnant, is not in conflict with Wilczek red-shifting [74] and non-monotonic mass loss of Bianchi-Smerlak [23], as the former occurs even when Domex is once again inertial and in the later, the non-monotonic mass loss occurs as long as the entropy approaches a constant (not necessarily zero).

We note that the entanglement entropy of the radiation on the left side of the mir- ror is negative. This is not unprecedented in the literature, however its interpretation is somewhat unclear. Bianchi, De Lorenzo, and Smerlak interpreted a negative entanglement entropy as the result of the radiation being less correlated than the vacuum [25]. On the other hand, Holzhey, Larsen, and Wilczek were of the opinion that negative renormalized entropy is the result of the radiation having more correlation than the vacuum [29]. We leave open the interpretation of our results, but it is interesting to note that for any fixed ξ, the positive entanglement entropy on the right side of the mirror exactly cancels the negative entanglement entropy on the left side. Therefore, the entanglement entropy of the radiation on the entire slice of any constant tis zero.

6 The correlations in the radiation

6.1 Correlation functions

An under-appreciated lesson stressed by Ford and Roman [76], is that there is a great deal more happening in the accelerating mirror geometry than is revealed by the expec- tation value of the stress-energy tensor alone. There are subtle increases or reductions in correlations between the flux along rays even where the expectation value vanishes. The stress-energy tensor correlation function is of interest in our situation because it reveals information about the energy flux that demonstrates the thermal character of the radiation above and beyond that of the thermal plateau of the stress-energy tensor during equilib- rium. The shock functions for the moving mirror are needed to compute the correlation functions for the stress-energy tensor. It was previously shown that the ray-tracing function p(u) is useful for delta-function pulse piece-wise mirror trajectories [76]. In this section, we extend this work to continuous trajectories and compute the correlations with an emphasis on the equilibrium period of Domex. The energy fluxes emitted by any moving mirror can be positive and negative, but they are only average values. The fluctuations around this average value are generally expected because the quantum state is not an eigenstate of the stress-energy tensor operator.

The correlation function for the stress-energy tensor is

C_{µνµ}^{0}_{ν}^{0} =hT_{µν}(y)T_{µ}^{0}_{ν}^{0}(y^{0})i − hT_{µν}(y)ihT_{µ}^{0}_{ν}^{0}(y^{0})i, (6.1)
where the spacetime points are indicated by y = (u, v) and y^{0} = (u^{0}, v^{0}). The correlation
functions between two right moving rays, two left moving rays, and right and left moving

## JHEP03(2017)013

rays are, respectively:

C_{RR}(u, u^{0}) =hT_{uu}(u)T_{uu}(u^{0})i − hT_{uu}(u)ihT_{uu}(u^{0})i, (6.2)
CLL(v, v^{0}) =hT_{vv}(v)Tvv(v^{0})i − hT_{vv}(v)ihT_{vv}(v^{0})i, (6.3)
C_{LR}(v, u^{0}) =hT_{vv}(v)Tuu(u^{0})i − hT_{vv}(v)ihT_{uu}(u^{0})i. (6.4)
Solved in terms of the ray tracing function, p(u), the results are [76]

C_{RR}(u, u^{0}) = [p^{0}(u^{0})p^{0}(u)]^{2}

8π^{2}[p(u^{0})−p(u)]^{4}, (6.5)
C_{LL}(v, v^{0}) = 1

8π^{2}[v^{0}−v]^{4}, (6.6)

CLR(v, u^{0}) = [p^{0}(u^{0})]^{2}

8π^{2}[p(u^{0})−v]^{4}, (6.7)

wherep^{0}(u) = dp(u)/du and p^{0}(u^{0}) = dp(u^{0})/du^{0}.

The above expressions deal only with correlations of distinct rays. These expressions simplify, as would be expected, in vacuum or with a static mirror present. For a static mirror we have the condition,v=p(u) =u, and

C_{RR}(u, u^{0}) =Cvac⊕static(u, u^{0}) = 1

8π^{2}[u^{0}−u]^{4}, (6.8)
C_{LL}(v, v^{0}) =Cvac⊕static(v, v^{0}) = 1

8π^{2}[v^{0}−v]^{4}, (6.9)
CLR(v, u^{0}) =Cstatic(v, u^{0}) = 1

8π^{2}[u^{0}−v]^{4}. (6.10)
In vacuumCLR(v, u^{0}) = 0 because there can only be correlations with left and right moving
fluxes with a mirror present. The correlation limits forC_{RR}andC_{LL}hold for either vacuum
or a static mirror, hence the xor, ⊕, in the subscript. The ratios

R1 ≡ C_{RR}(u, u^{0})

Cvac⊕static(u, u^{0}), (6.11)

and

R2 ≡ CLR(v, u^{0})

C_{static}(v, u^{0}), (6.12)

can tell us about enhancement and suppression of correlations. For Ri >1 one interprets
enhancement, forR_{i}<1 there is suppression.