Decreasing entropy of dynamical black holes in critical gravity

Critical gravity is a quadratic curvature gravity in four dimensions which is ghost-free around the AdS background. Constructing a Vaidya-type exact solution, we show that the area of a black hole defined by a future outer trapping horizon can shrink by injecting a charged null fluid with positive energy density, so that a black hole is no more a one-way membrane even under the null energy condition. In addition, the solution shows that the Wald-Kodama dynamical entropy of a black hole is negative and can decrease. These properties expose the pathological aspects of critical gravity at the non-perturbative level.


I. INTRODUCTION
It is known that the Minkowski vacuum in general relativity is dynamically stable against linear perturbations but the theory is not renormalizable, which is the main reason preventing perturbative quantization of gravity. However, if the quantum theory of gravity exists, it is natural to expect that there appear higher-curvature terms as corrections to general relativity in the action of its low-energy classical theory and the resulting field equations contain higher-derivative terms in general. In four dimensions, the coupling constants for the quadratic curvature terms are dimensionless in the units c = = 1 and such terms are dominant in the high-energy scale. For this reason, gravitation theories including quadratic curvature terms may be renormalizable [1][2][3]. (See [4] for a recent review on quadratic gravity.) However, in addition to renormalizability, unitarity should be required for classical theories to be quantized in a perturbative manner. Quadratic curvature theories admit two distinct maximally symmetric vacua in general, and usually there appear ghosts around both of them, which means that such theories are non-unitarity. In this context, Einstein-Gauss-Bonnet gravity is a well-known exceptional case, of which action consists of a special quadratic combination of the curvature tensors and the field equations do not contain higher-derivative terms. This theory is ghost-free around one of the maximally symmetric vacua which admits the general-relativistic limit [5,6]. However, this is the case only in higher dimensions because the Gauss-Bonnet term in the Lagrangian density becomes topological and the theory reduces to general relativity in four and lower dimensions.
Inspired by these results in three dimensions, a unitary quadratic curvature theory of gravity has been constructed in four dimensions, which is called critical gravity [14]. In spite that the field equations contain higherderivative terms, similar to BHT massive gravity, it is ghost-free around the AdS background [10,14]. Higherdimensional generalization of this critical gravity has been also achieved [15], in which the maximally symmetric vacua are not necessarily unique due to the contribution of the Gauss-Bonnet term in the action. Up to now, it is still not clear whether critical gravity and its higher-dimensional counterpart are renormalizable or not.
Although the maximally symmetric vacuum is not Minkowski but AdS in critical gravity, this is a remarkable classical theory holding unitarity. Then a natural question arises: Is the theory well-behaving also in the spacetime much different from the maximally symmetric one? This paper provides a negative answer to this question by constructing an exact solution representing an evolving black hole, defined by a future outer trapping horizon. More concretely, the solution represents a shrinking black hole by the injection of matter fields satisfying the null energy condition, which is never realized in general relativity. This shows that a black hole does not capture a concept of a one-way membrane under the energy condition in critical gravity. Furthermore, our solution shows that the entropy of dynamical black holes can decrease under the null energy condition. These properties exposes that the theory is pathological at the non-linear level.
The outline of the present paper is as follows. In Sec. II, we summarize the field equations in the most general quadratic curvature gravity in arbitrary n(≥ 4) dimensions and identify the parameter space for critical gravity. A definition of a dynamical black hole in terms of the trapping horizon is also explained. In Sec. III, we present several new Vaidya-type exact solutions for a null dust fluid together with a Maxwell field in the most general quadratic curvature gravity in four dimensions, which are compared with the corresponding solutions in general relativity and Einstein-Gauss-Bonnet gravity in arbitrary dimensions. In Sec. IV, we study the properties of dynamical black holes represented by our new solutions. Our conclusions and discussions are summarized in Sec. V. Einstein-Weyl gravity in arbitrary dimensions is explained in Appendix A. The details of computation to derive the Wald-Kodama dynamical entropy are presented in Appendix B. Our basic notation follows [16]. The convention for the Riemann curvature tensor is [∇ ρ , ∇ σ ]V µ = R µ νρσ V ν and R µν = R ρ µρν . The Minkowski metric is taken as diag(−, +, · · · , +), and Greek indices run over all spacetime indices. G n is the n-dimensional Newtonian constant. We adopt the units such that c = 1 and the four-dimensional Newtonian constant is described as G(:= G 4 ).

II. PRELIMINARIES
A. The most general quadratic curvature gravity In this section, we consider the most general quadratic curvature gravity in n(≥ 3) dimensions: where I m is the action for matter fields. Here α, β, and γ are coupling constants to the quadratic terms and L GB is the Gauss-Bonnet term defined by The resulting field equations are where the curvature tensor G µν is defined by and the energy-momentum tensor T µν for matter comes from the matter action I m . Here H µν is the quadratic curvature tensor defined by where The Gauss-Bonnet term is dynamical only for n ≥ 5 and hence H µν ≡ 0 holds for n ≤ 4.

B. Spacetime metric and maximally symmetric vacua
In the present paper, we consider the following Vaidyatype metric: where i, j = 2, 3, · · · , n − 1 and γ ij dz i dz j is the line element on the (n − 2)-dimensional maximally symmetric base manifold (K n−2 , γ ij ) with its curvature k = 1, 0, −1, namely the Riemann tensor (n−2) R ij kl on (K n−2 , γ ij ) is given by We assume that the base manifold K n−2 is compact for simplicity and hereafter V (k) n−2 denotes its volume. The metric function f (v, r) for the maximally symmet-ric vacuum solution is given by where λ is an effective cosmological constant and kλ = 0 is required. The spacetime is locally Minkowski, de Sitter (dS), and anti-de Sitter (AdS) for λ = 0, λ > 0, and λ < 0, respectively. The trace of the field equations (2.3) gives the following algebraic equation to determine λ: In four dimensions (n = 4), the quadratic terms do not affect the value of the cosmological constant and we have λ = Λ. In higher dimensions, the number of real solutions of Eq. (2.12) depends on the parameters and there can be two distinct maximally symmetric vacua. However, there are two cases which admit the unique vacuum. The first case is which gives the effective cosmological constant λ = Λ. The other case is (2.14) which gives λ = 2Λ.

C. Critical gravity
Critical gravity is described by the action (2.1) in four dimensions (n = 4) with a special choice of the coupling constants [14]. Eliminating massive scalar mode around the AdS background requires β = −3α and the condition for stable (non-tachyonic) massive spin-2 mode is 0 < α ≤ −1/2Λ with equality giving the massless spin-2 mode. Critical gravity is realized if spin-2 mode becomes massless, namely α = −1/2Λ. Finally, the relations between the coupling constants for critical gravity are In higher dimensions (n ≥ 5), the Gauss-Bonnet term comes into play and then unitary theory is realized for where λ is the (negative) effective cosmological constant determined by Eq. (2.12) [15]. This is the higherdimensional counterpart of critical gravity. In this higher-dimensional case, there are two free parameters α and Λ as coupling constants. If one assumes the condition (2.13) for the uniqueness of the maximally symmetric vacuum in addition, the relations between the coupling constants are where α is a single parameter as a coupling constant [15]. Actually, critical gravity and its higherdimensional counterpart with the relations (2.17) are special classes of the Einstein-Weyl gravity with a cosmological constant [14]. (See Appendix A.)

D. Definition of a dynamical black hole
In the following sections, we will study properties of the spacetime (2.9) representing a dynamical black hole. In a dynamical situation, a black hole is defined by a class of the trapping horizon [17]. Here we summarize the definition of a dynamical black hole described by the metric (2.9).
In the spacetime (2.9), radial null geodesics satisfy While ingoing radial null geodesics are represented by v =constant, outgoing null geodesics satisfy The tangent vectors along the future-directed radial outgoing and ingoing null geodesics, which are denoted respectively as k µ and l µ , are given by which satisfy k µ k µ = l µ l µ = 0 and k µ l µ = −1.
The surface area with constant v and r is given by n−2 r n−2 . The expansion along outgoing and ingoing radial null geodesics are computed as respectively, where we used Eq. (2.20). A trapping horizon is defined by the vanishing null expansion. In the present case, a trapping horizon is defined by Θ + = 0, and hence its location r = r h (v) is given by solving the following algebraic equation: A trapping horizon is classified in the following man- the ingoing radial null geodesic [17]. In this classification, a dynamical black hole is defined by a future outer trapping horizon [17].
Equation (2.22) shows that Θ − < 0 is always satisfied. On the other hand, from the following expression we obtain Therefore, a future outer trapping horizon is realized if the following condition is satisfied: Because the line element along the orbit of a trapping horizon r = r h (v) is given by where we used Eq. (2.19), the signature of the trapping horizon is determined by the sign of dr h /dv, independent of the theory. Therefore, the area of the trapping horizon increases (decreases) along its generator if and only if it is spacelike (timelike). If a future outer trapping horizon is timelike, it does not capture a concept of a black hole as a one-way membrane and therefore it should be non-timelike in order to define a black hole in a dynamical situation appropriately. In general relativity, for the spacetime with spherical (k = 1), planar (k = 0), or hyperbolic (k = −1) symmetry, it was shown that, under the null energy condition, a future outer (inner) trapping horizon is nontimelike (non-spacelike) and its area is non-decreasing (non-decreasing) along its generator [17,18].

A. Matter fields
In the present paper, we consider a null dust and a Maxwell field as matter fields, of which energymomentum tenor is given by Here T µν is the energy-momentum tensor for a Maxwell field, given by where F µν := ∂ µ A ν − ∂ ν A µ is the Faraday tensor and σ is a coupling constant. On the other hand, T µν is the energy-momentum tensor of a null dust fluid, given by where ρ is the energy density for a null dust and l µ is a null vector. In the coordinate system (2.9), we consider the null vector l µ for a null dust fluid in the following ingoing form: which gives T (2) r v = ρ. In the case of n ≥ 4, the form of the gauge field for the electric solution is given by where Q e (v) is a function of v. This expression gives and the only non-zero components of ∇ ν F µν is where a dot denotes the derivative with respect to v. Then, the non-zero components of the energymomentum tensor for n ≥ 4 are The conservation equations for the total energymomentum tensor ∇ ν T ν µ = 0 has only one non-trivial component for µ = v, which is written as where a prime denotes the derivative with respect to r. Now we are ready to present exact solutions in this system.

C. Einstein-Gauss-Bonnet gravity
In Einstein-Gauss-Bonnet gravity (α = β = 0) for n ≥ 5, there is the charged Vaidya-type solution given by Eqs. (3.10) and (3.11) with Eq. (3.13) and the following metric function: whereγ := (n − 3)(n − 4)γ. This solution with k = 1 has been obtained in [23] in a more general context. There are two branches of solutions corresponding to the sign in the metric function (3.14). While the solution with a minus sign (GR branch) admits the generalrelativistic limit γ → 0, the solution with a plus sign (non-GR branch) is diverging in this limit. For γ > 0, the maximally symmetric vacuum solution does not suffer from the ghost instability only in the GR branch [5,6].

D. New solutions in four-dimensional quadratic curvature gravity
In four dimensions (n = 4), the Gauss-Bonnet term becomes topological and therefore the most general quadratic curvature gravity becomes much simpler. In this case, new charged Vaidya-type exact solutions are available.

1.
Case β = 0 First let us consider the case with β = 0. The theory is then a special class of the so-called F (R) gravity [24], of which action and the field equations are where m(v) and Q e (v) are arbitrary functions. For β = 0 with 1 + 8αΛ = 0, on the other hand, there is the following dynamical solution in vacuum (ρ = Q e = 0): where m(v) and w(v) are arbitrary functions. With β = 0 and 1 + 8αΛ = 0, the function F (R) in the action (3.15) becomes a perfect square: Thus, not only the spacetime (2.9) with the metric function (3.19), but also any metric satisfying a single scalar equation R = 4Λ is an exact vacuum solution of the field equations (3.16) in this theory. For this reason, the theory with β = 0 and 1 + 8αΛ = 0 is singular among all the quadratic curvature theories in four dimensions.

Case β = 0
Lastly let us consider the case of β = 0. In this case, an exact solution is given by Eqs. (3.10) and (3.11) with , (3.22) where m(v) and Q e (v) satisfẏ In the limit of β → 0, this solution reduces to the solution (3.17) with Q e = 0. In this sense, the solutions (3.17) and (3.21) are two different branches of the charged solutions.

IV. BLACK-HOLE DYNAMICS IN THE NEW SOLUTIONS
In the spacetime (2.9), a future outer trapping horizon r = r h is given by f (v, r h ) = 0 with ∂f /∂r| r=r h > 0. In general relativity, under the null energy condition, a future outer trapping horizon is non-timelike and its area is non-decreasing along its generator [17,18]. Therefore, if the energy density of the null dust fluid (3.13) is nonnegative, the null energy condition is satisfied for the total energy momentum tensor T µν and then no pathological behavior is observed for dynamical black holes. In the charged Vaidya-type solution (3.10) and its generalization in Einstein-Gauss-Bonnet gravity (3.14), the energy density of a null dust is non-negative in the whole spacetime ifṁ ≥ 0 and ∂ v (Q 2 e ) ≤ 0 hold. However, different from general relativity, a pathological behavior of dynamical black holes is observed in in Einstein-Gauss-Bonnet gravity. In Einstein-Gauss-Bonnet gravity, a future outer trapping horizon is nontimelike (non-spacelike) and its area is non-decreasing (non-increasing) along its generator in the GR branch (non-GR branch) under the null energy condition [18,25]. This clearly shows that the non-GR branch is pathological and only the solutions in the GR branch are wellbehaving.
Nevertheless, it was shown that the Wald-Kodama dynamical entropy of the future outer trapping horizon, given by is the area of the trapping horizon, is non-decreasing along its generator in both branches under the null energy condition [18,25]. (See Appendix B for the definition of the Wald-Kodama dynamical entropy.) These results imply that the entropyincreasing law is more fundamental than the areaincreasing law in black-hole physics.
The universality of the entropy-increasing law rather than the area-increasing law has been observed also in the Vaidya-type solution in BHT massive gravity in three dimensions with a unique AdS vacuum [26]. However, it has been reported that the Wald-Kodama entropy of a dynamical black hole can decrease in BHT massive gravity in a vacuum solution with a certain relation between the coupling constants [27,28]. Now let us see the properties of a dynamical black hole represented by new solutions obtained in section III D in the most general quadratic curvature gravity in four dimensions.  First let us study the solution for β = 0. In the case with 1 + 8αΛ = 0, the location of the trapping horizon r = r h (v) is determined by f (v, r h ) = 0 with the metric function (3.17), namely The number of the future outer trapping horizons depends on the values of m and Q e and is shown by the result in [29]. Differentiating the above equation with respect to v, we obtain Because ∂f /∂r| r=r h > 0 holds on a future outer trapping horizon, see (2.26), the above equation shows that its area is non-decreasing (non-increasing) for 1 + 8αΛ > (<)0 under the condition ρ ≥ 0. This shows a pathological behavior of a dynamical black hole for 1 + 8αΛ < 0. Now let us see whether such a pathological behavior is observed in the dynamical entropy. The Wald-Kodama dynamical entropy of this black hole is given by The above expression shows that the dynamical entropy of the future outer trapping horizon is positive (negative) for 1 + 8αΛ > (<)0. However, the differentiation of Eq. (4.5) with respect to v giveṡ which shows that the entropy is non-decreasing under the condition ρ ≥ 0 independent of the sign of 1 + 8αΛ. This result provides another example that the entropy-increasing law is more fundamental than the area-increasing law. In the singular theory with β = 0 and 1 + 8αΛ = 0, on the other hand, the vacuum solution (3.19) contains two arbitrary functions m(v) and w(v). Therefore, the area of the future outer trapping horizon can decrease even in vacuum by choosing these functions appropriately. However, in contrast to the case of 1+8αΛ = 0, the dynamical entropy (4.5) of the black hole is identically zero, independent of m(v) and w(v). The results in this subsection are summarized in Table I.
Next let us see the time-evolution of the Wald-Kodama entropy. Differentiating Eq. (4.7) with respect to v, we (4.8) By κ TH > 0 and Eq. (B30), k−Λr 2 h > 0 holds for a future outer trapping horizon.
On the other hand, in the case of β < 0, Eq. (3.23) showsṁ < 0 (and henceȦ h < 0) and hence we assume 1 + 2Λ(4α + β) ≤ 0 andm ≥ 0 for ρ ≥ 0 everywhere. Then, because the first and the second terms in Eq. (4.8) are non-negative, the entropy is non-decreasing for Λ ≥ 0. The results obtained up to here are summarized in Table II. Now let us focus on critical gravity, which is realized for 1 + 2Λ(4α + β) = 0, β < 0, and Λ < 0. In this case, m < 0 holds by Eq. (3.23), which shows that the area of the future outer trapping horizon is decreasing and the Wald-Kodama entropy (4.7) is negative. Even worse, it is shown that the Wald-Kodama entropy can decrease under the null energy condition. By Eq. (3.22), ρ ≥ 0 requiresm ≥ 0. Then we consider the mass function m(v) = m 0 + m 1 v with m 0 > 0 and m 1 < 0. With this mass function, there is a certain domain of v admitting a future outer trapping horizon. In this case, we havë m = 0 and ρ = 0, so that the Wald-Kodama entropy is negative and decreasing only with a Maxwell field. These results certainly show pathological aspects of the theory at the nonlinear level.

V. SUMMARY AND DISCUSSIONS
In the present paper, we have obtained Vaidya-type exact solutions in the most general quadratic curvature gravity in four dimensions in the presence of a null dust fluid and a Maxwell field. These solutions represent a dynamical black hole defined by a future outer trapping horizon and we have studied their physical properties in the case with the positive energy density of the null dust.
Our main result is provided in critical gravity, which is the most important class of the theories in the present system. Our solution shows that the area of a future outer trapping horizon is decreasing by the injection of matter fields with positive energy density. This is never realized in general relativity and surely shows that a black hole does not capture a concept of a one-way membrane under the null energy condition in critical gravity.
Indeed, the violation of the area-increasing law has been observed also in our solutions with different coupling constants in the theory and such examples are known in Einstein-Gauss-Bonnet gravity [18] and BHT massive gravity with a unique AdS vacuum [26]. In these cases, however, the Wald-Kodama dynamical entropy of a black hole is non-decreasing under the null energy condition. In the case of critical gravity, in contrast, our solution shows that the Wald-Kodama entropy is negative and can decrease. These properties expose the pathological aspects of critical gravity at the non-perturbative level.
Then a natural question is whether the same is true or not in the higher-dimensional generalization of critical gravity [15]. This is quite nontrivial and worth pursuing because the Gauss-Bonnet term plays into the game in higher dimensions. We will address these problems elsewhere.
The definition of the Wald-Kodama dynamical entropy is Eq. (B5) with the Kodama vector K a instead of ξ µ , integrated over the trapping horizon [36]. κ in Eq. (B5) is then the dynamical surface gravity κ TH of the trapping horizon, defined by K b D [b K a] = κ TH K a evaluated on the trapping horizon.