Scattering of gravitational and electromagnetic waves off $AdS_2\times S^2$ in extreme Reissner-Nordstrom

The direct product of two-dimensional anti-de Sitter spacetime with a two-sphere is an exact solution of four-dimensional Einstein-Maxwell theory without a cosmological constant. In this paper, we analytically solve the coupled gravitational and electromagnetic perturbation equations of $AdS_2\times S^2$ in Einstein-Maxwell theory. On the other hand, $AdS_2\times S^2$ also describes the near-horizon region of the extreme Reissner-Nordstrom (ERN) black hole. We therefore also solve the connection problem: we show how the $AdS_2\times S^2$ perturbation equations arise from an appropriate near-horizon approximation of the corresponding equations for the ERN and then, using matched asymptotic expansions, we analytically extend the $AdS_2\times S^2$ solutions away from the near-horizon region connecting them with solutions in the far asymptotically flat region. From the point of view of ERN our results may be thought of as computing the classical scattering matrix for gravitational and electromagnetic waves which probe the near-horizon region of the black hole.


I. INTRODUCTION
AdS 2 is currently the focus of much activity in the context of two-dimensional quantum gravity in asymptotically anti-de Sitter spacetimes; see e.g. [1][2][3] and references therein. At the same time, AdS 2 has two major advantages over its higher dimensional counterparts in the AdS/CFT correspondence. The first advantage is that a direct product with a two-sphere produces an exact solution of four-dimensional pure Einstein-Maxwell theory without a cosmological constant, the so-called Bertotti-Robinson universe [4,5]. The second advantage is that the same solution also describes the near-horizon geometry of the asymptotically flat extreme Reissner-Nordstrom black hole; see e.g. [6]. This situates AdS 2 × S 2 in a privileged position for extending results produced in AdS/CFT investigations to the realm of fourdimensional classical and quantum gravity in asymptotically flat spacetimes. However, any such attempt requires that one first solves the connection problem: one needs to know how to extend near-horizon anti-de Sitter solutions to the far asymptotically flat region.
In this paper, we solve the connection problem for coupled gravitational and electromagnetic perturbations of AdS 2 × S 2 in Einstein-Maxwell theory. We show how the AdS 2 × S 2 perturbation equations arise from an appropriate near-horizon approximation of the corresponding equations for the full extreme Reissner-Nordstrom (ERN). We obtain analytically the exact solution to the AdS 2 × S 2 perturbation equations. We then find exact analytic solutions for two more approximations of the full ERN perturbation equations: an intermediate-region approximation whose solution is given by static perturbations and a far-region approximation whose solution gives the asymptotic behavior of the full ERN perturbations near infinity. Using the method of matched asymptotic expansions, we then glue the three solutions together and obtain the desired answer to our connection problem.
A reduction of the Reissner-Nordstrom perturbation equations to a set of two secondorder radial differential equations may be found in Chapter 5 of the monograph [7] and references therein; for a generalization to higher dimensions see [8]. In general, these radial equations can only be solved numerically. The method of matched asymptotic expansions has been used in the context of wave equations of (near-)extreme rotating black holes as early as [9][10][11]; for an application to the geodesic equations see [12]. Previous work indicating that ERN perturbations are at least partially amenable to analytic treatment includes [13,14]. This paper is organized as follows. Section II contains a telegraphic review of Reissner-Nordstrom, its extreme near-horizon limit, the decoupled AdS 2 × S 2 geometry, and the Regge-Wheeler-Zerilli gauge for the pertubation equations. In Section III we present a reduction of the ERN perturbation equations to a single fourth-order radial differential equation. This reduction is different from the standard one which produces two secondorder equations, but it contains the same information. In Section IV we begin by setting up the matched asymptotic expansions for the full ERN radial equation. We then derive the The case of near-extreme Reissner-Nordstrom and near-AdS 2 × S 2 is treated, to leading order in the deviation from extremality, in the companion paper [15].
The Reissner-Nordstrom solution of the Einstein-Maxwell equations (1) reads: Extreme Reissner-Nordstrom (ERN) is given by Q = M: The Bertotti-Robinson universe, which arises naturally as the near-horizon limit of ERN, may be obtained as follows. Make the coordinate and gauge transformation, to obtain 1 and then take the limit r ≪ 1 to get: 1 This solves the Einstein-Maxwell equations (1) on its own. The metric in (8) is From now on we set M = 1.
Spherical symmetry allows one to separate the angular dependence in the linearized Einstein-Maxwell equations (2-3) using scalar, vector, and tensor spherical harmonics labeled by (l, m), belonging to two sectors of opposite parity: "even" parity (−1) l and "odd" parity (−1) l+1 . In this paper, we will consider the even parity sector only because we are primarily interested in perturbations to the AdS 2 part of the near-horizon metric and the odd sector does not allow any such perturbations. 2 Due to the spherical symmetry one may also set m = 0 by an appropriate rotation. Time translation symmetry allows one to separate the time dependence as well using waves of definite energy ω. Finally, we move to the Regge-Wheeler-Zerilli gauge thereby putting the following ansatz for the metric and gauge field perturbations [16,17]: Note that modes with l ≥ 2 may be treated in a unified manner while the cases l = 0 and l = 1 are special and need to treated separately. 3 In this paper, we consider the l ≥ 2 modes.

III. REDUCTION OF THE PERTURBATION EQUATIONS
Putting the ansatz (9-10) into the linearized Einstein-Maxwell equations (2-3), on the background of the ERN (7), we may reduce them to a single fourth-order differential equation The expressions for the coefficients a i (r) may be found in App. A. The solution to this differential equation fixes the remaining components of the gravitational and electromagnetic perturbation according to: The reduction described above is not the standard Regge-Wheeler-Zerilli one, who reduce to two second-order equations, but it contains the same information. The reader may wonder what is the reduction path that leads to the above results. If we denote by E µν and M µ the linearized Einstein (2) and Maxwell (3) equations, respectively, then the reduction path may be described as follows. Begin by solving the equations E tr , E tθ , E rθ , E φφ − sin 2 θ E θθ which are algebraic equations for X, ψ, χ, V , respectively. This gives rise to (13)(14)(15)(16). Then, using (13)(14)(15)(16), equation E tt becomes algebraic for Y and yields (12). At this stage, given (12)(13)(14)(15)(16), one is left with equations E θθ , M t , M r , M θ for K (the remaining equations vanish identically).
However, one finds that M r , M θ are trivial multiples of E θθ while M t is a linear combination of E θθ and its derivative. This leaves only equation E θθ for K, which is equation (11).

IV. AdS 2 × S 2 ANSWERS AND THE CONNECTION PROBLEM SOLVED
Consider the scattering of gravitational and electromagnetic waves in the full ERN spacetime. Generic modes do not survive in the near-horizon limit. The modes which do survive and solve the AdS 2 × S 2 perturbation equations are low energy modes: In this regime, to leading order in ω, we may solve the scattering problem in the full ERN analytically using the method of matched asymptotic expansions as follows. Change variables in equation (11) according to and solve the resulting equation for H, by dividing the spacetime into three regions: Static: Far: The intermediate Static region is overlapping with both the Near and the Far regions.
Therefore, the Static solution may be used to connect the Near and Far solutions.
In the following, we will denote by b n i (r), b s i (r), and b f i (r) the coefficients of Eq. (19), in the Near, Static, and Far regions, respectively.

A. Near region
In the Near region, which corresponds to the AdS 2 ×S 2 throat, Eq.
m are the spherical Hankel functions of the first and second kind, respectively. 4 This Near solution is an exact solution with respect to the Bertotti-Robinson universe.
That is to say, using the perturbation ansatz (9-10) on the background of the Bertotti- and Eq. (18) is replaced by K(r) = r 2 H(r).

B. Static region
In the Static region, which corresponds to setting ω = 0, Eq.
The Static region overlaps with the Far region in Far-Static overlap: 1 ≪ r ≪ 1/ω (28) where Eq. (19) reduces to r 4 H ′′′′ + 2r 3 H ′′′ − 2l(l + 1)r 2 H ′′ + 2l(l + 1)rH ′ + (l − 1)l(l + 1)(l + 2)H = 0 and the solution is Expanding the Far solution (25) around the origin and the Static solution (24) around infinity, one may obtain linear relations between the C f i 's and C s i 's by matching the coefficients of the two expansions with the Far-Static solution (29).
Eliminating the C s i 's from the matching equations outlined above, we obtain the following linear relation between the C f i 's and C n i 's: where we have defined This is the main result of the paper and completes the solution to our connection problem.
The connection formulas (30) may also be thought of as computing the classical scattering matrix for gravitational and electromagnetic waves which probe the near-horizon region of extreme Reissner-Nordstrom.

V. A USEFUL BASIS OF SOLUTIONS
A useful basis of solutions for the full ERN equation (19) m (z) ∼ i m+1 z −1 e −iz this basis is defined by: From the connection formulas (30) we find that: H 1 has the Far amplitudes H 2 has the Far amplitudes H 3 has the Near amplitudes "up" solutions 5 one would define for ERN by infinitely oscillating phases at the horizon and infinity, respectively. For example, an "in" solution in ERN is defined as one that behaves like e iωr * near the horizon, where r * = −1/r + 2 ln r + r is the ERN tortoise coordinate.
On the other hand, the AdS 2 × S 2 tortoise coordinate is r * = −1/r so that the behavior of H 1 , H 2 near the AdS 2 × S 2 horizon agrees, for sufficiently small ω, with that of an "in" ERN solution everywhere near the horizon except precisely at the horizon where the two differ by the infinitely oscillating phase e 2iω ln r . Similar comments apply to the behavior at infinity.

VI. CONCLUSION
In this paper we have analytically solved the coupled gravitational and electromagnetic perturbation equations of the Bertotti-Robinson universe. Moreover, using matched asymptotic expansions, we have shown how to analytically extend these solutions to the asymptotically flat region of extreme Reissner-Nordstrom. We expect this extension to prove useful for transferring results from studies of AdS 2 holography to the realm of four-dimensional classical and quantum gravity in asymptotically flat spacetimes.
In has been argued that AdS 2 has no finite energy excitations [6]. The reason is that, with anti-de Sitter boundary conditions, backreaction in AdS 2 is so strong that it destroys its asymptotics. The reader might therefore wonder how do the results of this paper fit in that picture. We note that it is possible to study the backreaction problem using the linearized perturbations of AdS 2 × S 2 that we have explicitly found in Section IV A. The technique uses the so-called "linearization stability constraints" and we expect that, with anti-de Sitter boundary conditions, one would confirm that the solutions of Section IV A should be discarded. Indeed, we expect that the only solution which obeys asymptotically AdS 2 × S 2 boundary conditions is diffeomorphic to AdS 2 × S 2 itself; see e.g. [21]. However, the main focus of this paper is the connection with the asymptotically flat extreme Reissner-Nordstrom and in this context "leaky boundary conditions" at the location of the would-be to verify (see e.g. [32]) that, up to the SL(2, R) isometries of AdS 2 , the only solution to the Schwarzian action expanded to second order in ǫ is given by ǫ(t) = αt 3 with α ∝ δM − δQ.

ACKNOWLEDGMENTS
I am grateful to Sam Gralla and Gary Horowitz for useful conversations. This work is supported by NSF grant PHY-1504541 6 For readers who are familiar with the NHEK geometry [22] in the extreme Kerr throat, we note that the situation here is exactly analogous to the one in Kerr/CFT [23]. Linearization stability constraints imply that, up to diffeomorphisms and boundary gravitons, asymptotically NHEK boundary conditions are consistent only with trivial solutions h µν = 0 [24,25]. On the other hand, with astrophysically meaningful boundary conditions imposed at future null infinity of extreme Kerr, Refs. [26,27] analytically computed the gravitational wave signals from extreme-mass-ratio-inspirals in NHEK.