Static BPS black holes in AdS4 with general dyonic charges

We complete the study of static BPS, asymptotically AdS4 black holes within N\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$ \mathcal{N} $$\end{document} =2 FI-gauged supergravity and where the scalar manifold is a symmetric very special Kähler manifold. We find the analytic form for the general solution to the BPS equations, the horizon appears as a double root of a particular quartic polynomial whereas in previous work this quartic polynomial further factored into a pair of double roots. A new and distinguishing feature of our solutions is that the phase of the supersymmetry parameter varies throughout the black hole. The general solution has 2nv independent parameters; there are two algebraic constraints on 2nv + 2 charges, matching our previous analysis on BPS solutions of the form AdS2× Σg. As a consequence we have proved that every BPS geometry of this form can arise as the horizon geometry of a BPS AdS4 black hole. When specialized to the STU-model our solutions uplift to M-theory and describe a stack of M2-branes wrapped on a Riemman surface in a Calabi-Yau fivefold with internal angular momentum.


Introduction
The study of BPS black holes in flat space has provided important insights into the nature of quantum gravity [1] and it is natural to search for a similar understanding of BPS black holes in asymptotically AdS space. Indeed there is hope that one might ultimately be able to use the holographic duality of the background AdS space [2][3][4] to understand the dynamics of black holes and these holographic dualities are certainly under the best control for supersymmetric theories.
Whereas the complete solution for asymptotically flat BPS black holes in four dimensional N = 2 ungauged supergravity was found some time ago [5,6] it is only somewhat recently that there has been progress in charting out the solution space of asymptotically AdS 4 static BPS black holes in gauged N = 2 supergravity. In this work we complete the study of the solution space of static BPS black holes in N = 2 FI-gauged supergravity. 1 To be more precise we require that the vector-multiplet scalar manifold M v is homogenous and very special Kähler or in other words that it is a coset and that there is a symplectic duality frame where the prepotential is cubic.
A notable development in this field was the solution of Cacciatori-Klemm [7] who studied a restricted set of background charges in the STU-model and found a class of solutions depending on four charges with one constraint, leaving a three-dimensional solution space. 2 This constraint is a BPS refinement of the Dirac quantization condition due to the charged 1 FI-gauged supergravity refers to the Fayet-Iliopoulos gauging, namely where the U(1)R ⊂ SU(2)R is gauged. 2 This solution was further studied in [8,9].

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gravitini and is of course absent in ungauged supergravity and the study of asymptotically flat black holes.
We have recently considered [10] these general N = 2 FI-gauged supergravity theories and exactly solved the BPS conditions for geometries of the form AdS 2 × Σ g where Σ g ∈ S 2 , R 2 , H 2 is (a covering space of) a Riemann surface of genus g. We found that the entropy of the solution is related to the famous quartic invariant of special geometry and indeed this invariant will prove to be indispensable in our current analysis as well. An interesting result from the analysis of horizon geometries was that the solution space is 3 2n v -dimensional; there are n v + 1 magnetic charges p Λ , along with n v + 1 electric charges q Λ and there are two constraints from the BPS conditions. One constraint is the Dirac quantization condition mentioned earlier but in addition there is another constraint given by (3.25) below. Consequently it was conjectured that the solution space of BPS black holes is also 2n v -dimensional. In this work we prove this conjecture by constructing these solutions explicitly.
In previous work we have generalized the solution of [7] in two ways; for theories with a symmetric very special Kähler scalar manifold we presented axion-free solutions which depend on n v independent charges and give the CK solution when restricted to the STU model. In addition, in [11] we showed how to use unbroken duality symmetries to generate two new charges in the STU-model. For the STU-model in particular, this gives a fivedimensional solution space whereas the analysis of [10] predicts that there should be a six-dimensional solution space. Recently it was shown [12] that this family of solutions with non-trivial axions can be generalized from the STU-model to theories where M v is a symmetric very special Kähler manifold but still, the dimension of the solution space was 2n v − 1, one less than conjectured in [10]. The final dimension of the solution space indeed exists as we constructively prove in the current work.
This paper is organized as follows. In section 2 we review the BPS equations and outline our ansatz. In section 3 we present our solution to the BPS equations. In appendix A we summarize various details of special geometry which are needed for the current work.

The equations and the Ansatz
The standard ansatz for static AdS 4 black holes is where dΣ 2 g is the uniform metric on S 2 , T 2 , H 2 with corresponding curvature κ = (1, 0, −1). The scalar fields are radially dependent z i = z i (r) and the gauge fields just contribute through the conserved charges where the dual field strength is given by

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The charges and gauging parameters 4 are naturally assembled into symplectic vectors A static BPS AdS 4 black hole amounts to a domain wall interpolating between AdS 4 in the UV to AdS 2 × Σ g in the IR, the effective cosmological constant varies along this flow due to the non-trivial profiles for scalar fields which contribute to the cosmological constant through the scalar potential. For a particular G and Q in the STU-model, 5 in [7] the equations for 1 4 -BPS black holes were found to simplify considerably and the exact solution was found. These solutions can be lifted in M-theory and interpreted as wrapped M2-branes along the lines of the work of Maldacena-Nunez [13]. Indeed restricted classes of such wrapped M2-branes had already been considered numerically in [14] but the solution of [7] was the first exact supergravity solution 6 in any dimension of a stack of wrapped branes which has an AdS factor in the IR.
In four dimensions one has available the tools of special geometry and in [8] a duality covariant form of the BPS equations was derived: 7 where ψ is the phase of the supersymmetry parameter and we have defined the standard symplectic scalars In addition one must impose the Dirac quantization condition specialized for these BPS equations: The equation (2.6) is a real symplectic vector with 2n v + 2 components which can be extracted by contracting (2.6) with V, V, D i V, D ı V . In this way, one obtains differential equations for the phase ψ, the metric mode e U and the n v complex scalars z i . Comparing the resulting equation for ψ with (2.8) one obtains the algebraic constraint The gravitini are charged with respect to the U(1) gauge fields A Λ µ by G, it is always possible to find a symplectic frame where these couplings are purely electric and so the gravitini are just minimally coupled to the A Λ µ . 5 In the symplectic frame where the gauging parameters are purely electric, the charges studied in [7] were purely magnetic. 6 We are excluding the elementary solutions with constant scalar fields which for four dimensional black holes were considered in [15]. 7 We use the standard notation for the sections

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which can then be enforced at the expense of (2.8). To be clear, an equivalent complete set of BPS conditions is (2.6), (2.7), (2.10), (2.11) and this is the set we will solve in the next section. It may be interesting to note that the constraint (2.11) is a generalization of the constraint 0 = Im e −iψ Z found for single-center half-BPS black holes in ungauged supergravity [16]. Using these equations, the analytic solution of [7] was generalized to theories where M v is a symmetric very special Kähler manifold in [17]. In these examples, the axions vanish identically and the complex symplectic sections become either real or imaginary leading to a sharp simplification of the equations (2.6)-(2.7) and in these example both sides of (2.11) vanish identically. The solutions of [17] are parameterized by n v charges out of the 2n v + 2 components of Q and in [11] it was observed that one can use unbroken duality symmetries to generate axions.
The BPS equation (2.6) was recently refined in [12] using the quartic invariant I 4 and its derivative, 8 which further simplifies the analysis of the models with general gauging parameters G and charges Q. Specifically, using the identity (A.19) one immediately finds that (2.6), (2.7) and (2.11) become The key step in arriving at (2.12) is to remove the pesky ΩMG and ReV terms in (2.6) leaving an equation purely in terms of Im V and e V . The main result of the current work is to solve (2.12)-(2.14) in complete generality subject to the boundary conditions of AdS 4 in the UV and AdS 2 × Σ g in the IR.
The key insight of Cacciatori and Klemm in [7] was the ansatz for e V : where R is the radius of AdS 4 and v 0 > 0. In (2.16) e V is completely fixed by the UV and IR boundary conditions whereas in principle e V could be a power series in 1 r and indeed that is what we will find. 9 In this work we generalize (2.16) to the following ansatz 10 (2.17) Clearly e 2V has a double root at r = 0, a familiar feature of charged extremal black holes namely that the two horizons coincide, the remaining two roots however need not coincide.

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The ansatz for Im V requires further inspiration, we find that the following is ultimately justified by our success: where A i are the symplectic vectors which will be explicitly solved for.
3 The solution

The general solution
When evaluated on the ansatz (2.17) and (2.18) and expanded order by order, the BPS equation (2.12) yields where we have used the solution to (2.13) The constraint (2.14) expanded order by order in r gives It should be noted that this whole system of equations is vastly overdetermined and for a solution to exist the system must be highly redundant. One starts solving this system by first re-analyzing the UV (3.1) and IR (3.5), (3.10) but the intermediate equations involve A 2 in nontrivial ways. The UV boundary conditions for AdS 4 provide A 3 as the solution to (3.1) and one finds where we have appealed to the analysis of [17] to fix the overall normalization. The BPS equations are non-linear in terms of the A i and are somewhat challenging to solve directly. Making use of the various relations contained in appendix A.2 we have found the following explicit solution: .

(3.16)
Our solution for A 2 is somewhat more complicated, the ansatz is the same as for A 1 and we find that the constants b j are given by where we have defined Note that the BPS equations have a symmetry A 2 → −A 2 and as such the overall sign of b 3 in our expressions is undetermined by the BPS conditions and must be fixed by demanding regularity of the solution. A priori one might have expected that the ansatz for A i involved terms proportional to the symplectic vectors G and Q, we have considered such terms and found their coefficients to vanish. With these expressions for A i we get the following result for the expansion of e V : Since this constraint is independent of the radius it must be imposed on the whole black hole. We find that with this constraint enforced, the above solution solves each of (3.7)-(3.10). The expressions above for {a i , b j , v k } have been evaluated subject to (3.25) although in principle one could have used (3.25) to eliminate I 4 (G, G, Q, Q).
We have used what we find to be a more concise presentation. We emphasize that solving for Im V constitutes a complete solution of the problem, from which the metric functions e U , e V , the scalar fields z i and the phase of the supersymmetry parameter ψ can all be obtained as follows. Using the identity (which follows from (A.19) evaluated with A → Im V): we find (3.27) Having the expression for the complex sections V it is straightforward to read off the complex scalar fields: Contracting (3.27) with Im V we get the remaining metric function from The phase of the supersymmetry parameter ψ can be extracted from and is generically non-constant as opposed to all previous solutions in [7,11,12,17] where the supersymmetry phase is constant. Note that the numerical solution presented in [18] for gauged supergravity with hypermultiplets also has a non-constant phase for the spinor. While the explicit solution (3.13)-(3.16) and (3.18)-(3.21) is satisfying in the sense that it is exhaustive within the class of theories considered, its explicit form is not exactly edifying. The crucial step in finding these solutions was starting from the metric ansatz in (2.17), which for various reasons this was incorrectly excluded in [12]. It seems plausible that using the tools of special geometry one could find a a more concise representation of this solution, which may possibly be required for this solution to have applications to generalizations discussed in the introduction.

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3.2 The limit I 4 (G, G, G, Q) = I 4 (G, Q, Q, Q) = 0 To observe the limit I 4 (G, G, G, Q) = I 4 (G, Q, Q, Q) = 0, it is useful to note that the constraint (3.25) implies which is finite in this limit. We find the following explicit expressions This limit corresponds to those solutions which can be obtained by a duality transformation from the solutions in [17], a distinguishing feature is that the phase of the supersymmetry parameter (which is duality invariant) is constant.

Conclusions
We have solved the general static BPS black hole in N = 2 FI-gauged supergravity and found that the full solution depends on 2n v out of 2n v + 2 charges. The two constraints are given by the BPS Dirac quantization condition (2.10) as well as (3.25), where the latter has its origin in (2.11). When restricted to the STU-model, all these solutions lift to Mtheory via an embedding [19] of the STU-model into the N = 8 de-Wit Nicolai theory [20]. In principle this uplift is known [21,22] but in practice it is quite complicated. Simple formulae for this uplift are available in [19] for the STU-model when the axions vanish but our solutions have non-trivial axions and there is thus no simple uplift formula. In the symplectic frame discussed in [17] the magnetic charges uplift to Chern numbers of fibration of S 7 over Σ g (the structure group of the S 7 bundle is reduced from SO(8) to U(1) 4 ) whereas in this frame the electric charges lift to angular momentum around circles in S 7 .

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While our results are limited to BPS black holes, a solution for (not necessarily BPS) asymptotically AdS 4 black holes in the STU-model was presented in [23] depending on all eight charges. This was performed with a view towards embedding these black holes in the N = 8 theory 11 using the embedding of [19]. In principle the solutions of the current work, when restricted to the STU-model should be contained in [23] but establishing this map does not appear to be straightforward. Presumably making this connection clean would aid our understanding of these solutions in general.
We hope that the solution obtained in this work will shine light on the construction of more general BPS black holes in gauged supergravity. One might find a useful a comparison to the work of Demianski-Plebanski [32] where they found a very general black hole solution to the Einstein-Maxwell theory depending on mass, nut charge, electric and magnetic charge as well as rotation and acceleration, with and without a cosmological constant. This remarkable solution unified a slew of existing works in one framework (see [33] for the most recent analysis of the supersymmetry of the PD solution). It seems to be a reasonable hope that a similar solution but with non-constant scalars can be obtained in FI-gauged supergravity, at least in the BPS sector, and we hope that the methods employed in this work, which maintain the full symmetries of the theory will be useful in this regard. 12 Having said that, one should keep in mind an interesting feature which emerged in the work [23]; while the full black hole solution space is continuously connected, allowing for a tuning to zero of the cosmological constant, the BPS sector is not. To pass continuously from a BPS asymptotically AdS 4 black hole to a BPS asymptotically flat black hole, one must pass through the non-BPS sector.
We also have in mind black holes in theories with hypermultiplets [18]. Hypermultiplets do not add any charges, although they may give mass to vector fields, in a sense they are just an additional scalar field sector, and as such one might hope that ultimately there are analytic solutions analogous to those presented here with non-trivial profiles for the hyper-scalars. This would have interesting applications since the M-theory lift of the many known N = 2 gauged supergravities with hypermultiplets often involve wrapped M5 branes in addition to wrapped M2-branes [38,39]. There are also known embeddings into M-theory of such theories which just contain the dynamics of M2-branes [40].

A.1 Generalities
We will use the conventions where the prepotential is given by and the covariant tensor is given by and any symplectic vector can be expanded in these sections. For example the charges are expanded as We also have a complex structure on the symplectic bundle over M v : where .11) and N = R + iI is the standard matrix which gives the kinetic and topological terms in the action for the gauge fields.