On the oscillation of species

Journal of High Energy Physics, Sep 2014

We describe a new class of BPS objects called magnetubes: their supersymmetry is determined by their magnetic charges, while their electric charges can oscillate freely between different species. We show how to incorporate these objects into microstate geometries and create BPS solutions in which the charge densities rotate through different U(1) species as one moves around a circle within the microstate geometry. Our solutions have the same “time-like” supersymmetry as five-dimensional, three-charge black holes but, in various parts of the solution, the supersymmetry takes the “null” form that is normally associated with magnetic charges. It is this property that enables the species oscillation of magnetubes to be compatible with supersymmetry. We give an example in which the species oscillate non-trivially around a circle within a microstate geometry, and yet the energy-momentum tensor and metric are completely independent of this circle: only the amplitude of the oscillation influences the metric.

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On the oscillation of species

Iosif Bena 3 Simon F. Ross 1 Nicholas P. Warner 0 2 3 0 Institut des Hautes Etudes Scientifiques , 91440 Bures-sur-Yvette, France 1 Centre for Particle Theory, Department of Mathematical Sciences, Durham University , South Road, Durham DH1 3LE, U.K 2 Department of Physics and Astronomy, University of Southern California , Los Angeles, CA 90089, U.S.A 3 Institut de Physique Theorique , CEA Saclay, CNRS-URA 2306, 91191 Gif sur Yvette, France We describe a new class of BPS objects called magnetubes: their supersymmetry is determined by their magnetic charges, while their electric charges can oscillate freely between different species. We show how to incorporate these objects into microstate geometries and create BPS solutions in which the charge densities rotate through different U(1) species as one moves around a circle within the microstate geometry. Our solutions have the same time-like supersymmetry as five-dimensional, three-charge black holes but, in various parts of the solution, the supersymmetry takes the null form that is normally associated with magnetic charges. It is this property that enables the species oscillation of magnetubes to be compatible with supersymmetry. We give an example in which the species oscillate non-trivially around a circle within a microstate geometry, and yet the energy-momentum tensor and metric are completely independent of this circle: only the amplitude of the oscillation influences the metric. 1 Introduction Merging the two types of supersymmetry 2.1 Time-like and null supersymmetry of M2 and M5 branes 2.2 The classic solutions with time-like supersymmetry 2.3 Merging the two classes of supersymmetry 2.4 A degenerate limit and a class of null BPS solutions 3 Supergravity coupled to four vector multiplets 3.1 The supergravity action 3.2 The supersymmetry conditions 3.3 Adding species on the T 4 4 Solutions in six and ten dimensions 4.1 Lifting to six dimensions 4.2 The ten-dimensional IIB configuration 5 7 5.1 AdS3 S2 5.2 Adding the supertube/magnetube 5.3 Regularity near sources 5.4 Geometry of the regular magnetube 5.5 AdS3 S3 asymptotics at infinity 5.6 Global regularity 6 Species oscillation 6.1 Some simple oscillating solutions 6.2 Regularity 6.3 Solutions with a -independent metric The oscillating modes 7.1 The Greens function 7.2 The Fourier modes 7.2.1 The explicit modes 7.2.2 On-axis limit 7.2.3 Examples 7.3 Asymptotics of the modes at infinity 1 2 5 Conclusions 8.1 Comments on supersymmetric species oscillation 8.2 Non-BPS, asymptotically flat solutions 33 33 34 Introduction Microstate geometries play a double role in the study of solutions in supergravity. First, microstate geometries involve a mechanism that supports time-independent, smooth, solitonic, horizonless solutions within massless supergravity theories and so such solutions can potentially represent completely new classes of end-states for stars. The second role is that there are vast classes of such solutions and these classes come with extremely large moduli spaces. As a result, the fluctuations of microstate geometries can capture a significant portion of the microstate structure of the black hole that possesses the same asymptotic structure at infinity. To understand the extent to which such classical solutions can capture microstate details it is important to understand and classify the moduli spaces of solutions and find all the ways in which such solutions can fluctuate. This has been the focus of much recent work and in this paper we will exhibit a new and broader class of BPS fluctuations that we call species oscillation. The key building block of solutions with species oscillations is a new object of string theory, which we will call the magnetube. The magnetube has M5 and momentum charges (which are magnetic in five dimensions), as well as several electric M2 charge densities that can oscillate between positive and negative values along the M5-P common direction. The original motivation for studying this object, and species oscillation in general, was the idea that it can be used to create microstate geometries for Schwarzschild (electrically neutral) black holes [1]. The specific magnetube considered in [1] involved a KK-monopole with (NS5, D5) charge specified by a vector at each point along a line in the KKM worldvolume. This charge vector rotates in the (NS5, D5) charge space as one goes around this line so that the resulting configuration has no overall (NS5, D5) charge. At each point on the line the configuration looks like a piece of a BPS supertube, but at different locations the D5 charge of this object can have opposite signs, and so it does not preserve any supersymmetry associated with these charges. Our first result is to show that the object found in [1], as well as the class of M5-P magnetubes that we construct in this paper, are secretly supersymmetric. Normally one does not expect this, because the negative and positive M2 (or D5) charge densities at two different locations will attract and will generically want to collapse into each other. However, the story is much richer: because of the presence of extra species one can arrange the M2-brane densities so that, at each point along the direction in which the charge densities vary, the Killing spinors are those of the (magnetic) M5 branes and momentum, and are not affected at all by the presence of (electric) M2 branes. Hence, the physics of the magnetube is the mirror of the physics of normal supertubes [2]: for the magnetube the magnetic (M5 and P) charges control the supersymmetry, and the contributions of the fluctuating electric charges to the Killing spinor equations cancel; for normal supertubes the (electric) M2 branes control the supersymmetry and the (magnetic) M5 and momentum charges can fluctuate arbitrarily, as their contribution to the Killing spinor equations cancel each other. The original spirit of [1] was to try to bend the infinite magnetube with oscillating species (whose solution they constructed) into a round magnetube, which would be neutral and hence give microstate geometries for the Schwarzschild black hole. It is clear that this would break the supersymmetry of the infinite magnetube, as the resulting configuration will have mass and no charge. However there is also an indirect and more useful way to see how supersymmetry is broken: bending an infinite tube in R3 S1 into a round one in R4 can be realized by adding a Taub-NUT center to the solution and bringing this center close to the tube (in the vicinity of the Taub-NUT center the metric is R4). For normal supertubes this procedure is supersymmetric [35], because the Killing spinors of the Taub-NUT space are compatible with the M2-brane Killing spinors of the supertube. However, the magnetube has M5 and P Killing spinors, and those are not compatible with the Taub-NUT ones,1 and hence trying to create a neutral configuration results necessarily in the breaking of the supersymmetry preserved by the infinite magnetube solution. Our second result is to find a way to embed M5-P magnetubes into some of the known supersymmetric solutions and to obtain new classes of BPS solutions with species oscillation. Using magnetubes and species oscillation to create more BPS solutions may appear contrary to the original spirit of [1], which proposed these objects as building blocks for non-extremal microstate geometries. However, this is not so: our result strengthens the evidence for the existence of magnetubes, and proves that there is no obstruction to bending them, and hence to using them in principle for the purpose originally intended in [1]. Embedding a magnetube into a supersymmetric solution that has M2 Killing spinors may, at first, seem impossible because the magnetic Killing spinors of the magnetube are not compatible with the electric M2 Killing spinors preserved by the background. Specifically, given a Killing spinor, , one can define the vector K = and this is always a Killing vector that represents the time-translation generated by the anti-commutator of two supersymmetries. In electric BPS solutions this Killing vector is time-like and in magnetic BPS solutions this Killing vector is null: we therefore use the terminology time-like or null supersymmetry to refer to these two distinct and apparently incompatible classes. One can also verify that the supersymmetry projectors associated with the underlying magnetic and electric charges are also incompatible because the projectors do not commute with one another. On the other hand, when lifted to six dimensions all supersymmetric solutions give rise to null Killing isometries and so, from this perspective, there should be some possibility of interpolation between such supersymmetries. Indeed, even in five dimensions there is a crucial loop-hole in the structure of the electric BPS supersymmetries: the four-dimensional spatial bases are allowed to be ambi-polar, which implies that while the Killing vector associated with the supersymmetry is time-like almost everywhere (and particularly at 1One can see this easily by compactifying to type IIA string theory, where the Taub-NUT space becomes a D6 brane, and the M5 and P become D4 and D0 branes respectively. infinity), there are critical surfaces, where the signature of the base space changes from (+, +, +, +) to (, , , ), and where the Killing vector becomes null. We will show that the usual time-like supersymmetries of electric charges actually get infinitely boosted and become magnetic or null supersymmetries on the critical surfaces. It is therefore possible to introduce species oscillation on magnetubes localized right on top of a critical surface, where the Killing spinors of the background become magnetic and are therefore compatible to those of the magnetubes, preserving supersymmetry globally. Besides establishing the existence of magnetubes as fundamental building blocks of black hole microstates, the new families of supersymmetric solutions that we construct are interesting in their own right. For example, in four dimensions the uniqueness theorems are very stringent but in five and six dimensions there are huge families of microstate geometries with the same asymptotic charges. It is thus interesting to explore the range of possibilities and our new classes of solution will have electric fields that fluctuate and yet the metric either does not fluctuate at all, or the fluctuation response is locally suppressed due to coherent combinations of fluctuating charge densities. This class of solutions is, in this sense, similar to Q-balls [6, 7]. The latter solutions are supported by time-dependent matter fluctuations arranged so that the energy-momentum tensor and hence the metric are both time-independent. The solutions we construct here are not time-dependent but the fields fluctuate as a function of some S1-coordinate, , and yet the energy-momentum tensor and metric can be arranged to remain invariant along . More generally, one can arrange the fields to fluctuate in such a way that the leading-order perturbations to the energy-momentum tensor near the source remain -independent with the fluctuations only becoming visible at sub-leading orders. We will formulate species oscillation in five-dimensions using a T 6 compactification of M-theory that is essentially described in [8]. There will be one spectator M2 brane wrapping a fixed T 2 and the species oscillation will take place between four classes of M2branes that wrap the remaining T 4 in different ways. One can also reduce this to IIA by compactifying on an S1 inside the T 2 of the spectator M2, converting it to an F1 string while the oscillating M2s become oscillating D2s. If one T-dualizes on the circle wrapped by the F1, one obtains a IIB compactification in which the F1 has become momentum charge and the oscillating species are simply three sets of D3-branes that intersect along a common circle while wrapping the T 4 in exactly the same manner as the original M2s. The importance of the IIB frame is that it is only in this frame that our solutions will be completely smooth microstate geometries. Our formulation also has the advantage of having all the oscillating species originating from the same type of branes. It is also possible to relate some of our magnetube solutions to the smooth IIB frame magnetubes obtained in [1], by a duality sequence that we will discuss in section 4.2. In section 2 we discuss the two classes, time-like and null, of supersymmetry and their relation to electric and magnetic BPS solutions in M-theory. We also show how both types of supersymmetry can be present in BPS solutions with ambi-polar base metrics. In section 3 we discuss the relevant five-dimensional N = 2 supergravity theories and their origins in M-theory. In section 4 we discuss the six-dimensional uplifts and their relation to IIB supergravity. We also discuss the regularity conditions that make supertubes into smooth microstate geometries in six dimensions. Section 5 contains a template microstate geometry which is a standard, non-oscillating microstate geometry with two Gibbons-Hawking (GH) geometric charges and a supertube on the critical surface between the GH charges. In reality this supertube is actually a magnetube because it preserves a null supersymmetry. Indeed, the constructions of supertubes and magnetubes are mathematically parallel and, following the logic of section 2, one can think of magnetubes as infinitely-boosted supertubes. In section 5 we also check the regularity and asymptotic structure of this magnetube solution. In section 6 we introduce species oscillation into the template magnetube and give an example in which the metric does not oscillate. We also see that the metrics of the oscillating solutions are almost identical to those of the template solutions and are therefore regular. In section 7 we give details of the Greens functions and explicit mode functions that are the essential, though technical, part of our solutions with species oscillation. While our examples involve only very simple microstate geometries, they will nevertheless provide a good local model of what we expect from species oscillation in a generic bubbling solution. Finally we make some concluding remarks in section 8. Merging the two types of supersymmetry In this section we illustrate one of the key ingredients of species oscillation: the fact that one can mix both time-like and null supersymmetric components within a single, fivedimensional solution. We will assume some familiarity with the five-dimensional microstate geometries that have been constructed over the last few years. One can find discussions of this in, for example, [1821]. In section 3 we will discuss the general form of five-dimensional N = 2 supergravity coupled to an arbitrary number of vector multiplets and this can also serve as something of a review of the relevant supergravity structure but in greater generality than is needed to understand the merging of the two types of supersymmetry. Since the latter idea is something rather new, we have chosen to show how it works here first before diving more deeply into the technicalities of the more complicated supergravity theories that are needed to implement species oscillation. For newcomers to the microstate geometry program it might be useful to review section 3 first. Time-like and null supersymmetry of M2 and M5 branes In both eleven-dimensional and five-dimensional supergravity there are two distinct classes of supersymmetry, which are classified by whether the associated time translation invariance is actually time-like or null. More precisely, if is the residual supersymmetry then the vector is necessarily a Killing vector, and it can either be time-like or null [9, 10]. It is relatively easy to see that the vector is dominated by its time component because, in frame indices, one has 0 = . To investigate the other components one needs to know a little more about the structure of the supersymmetry. One the simplest descriptions of BPS three-charge black holes in five dimensions is obtained by compactifying eleven-dimensional supergravity on a six-torus, T 6. The charges are then carried by three sets of mutually BPS M2-branes and thus the supersymmetries obey the projection conditions = , where the five-dimensional space-time is coordinatized by (t = x0, x1, x2, x3, x4) and the T 6 is coordinatized by (x5, . . . , x10). The microstate geometries corresponding to such black holes are, by definition, required to have the same supersymmetries, in that they also satisfy (2.2). One should also note that because 01...9 10 = , the conditions (2.2) also imply = , which constrains the holonomy of the spatial base. One can now insert the 0cd into (2.1) and commute through the a. The fact that a, for a 6= 0, anti-commutes with at least one of the 0cd means that a = 0 for a 6= 0 and so the Killing vector for such black holes and their microstate geometries is necessarily time-like. The BPS three-charge black holes and their microstate geometries are dominated by their electric charge structure but can carry non-zero, dipolar magnetic charge distributions whose fields fall off too fast to give any net charge at infinity. There is a simple magnetic dual of this picture in which the M2 branes are replaced by M5 branes. We will take the M5 branes to have a common direction, = x4, which, for the present, will be flat and either infinite or a trivially fibered S1. The M5-brane supersymmetries obey the projection conditions = , = . Again one can insert the 0 into (2.1) and commute through the a and conclude that a = 0 for a 6= 0, . Moreover (2.5) implies 0 = and so the Killing vector is necessarily null. Thus these systems of M2 branes and M5 branes are exemplars of the two classes of supersymmetric systems in five and eleven dimensions. For our purposes, it is important to note that, just as the BPS three-charge black holes and microstate geometries can be given non-zero, dipolar magnetic charge distributions whose fields fall off too fast to give any net charge at infinity, the M5 brane system can be given non-zero, dipolar electric charge distributions whose fields fall off too fast to give any net charge at infinity. In this way one can make BPS magnetubes that have no net electric charge and this observation will lie at the heart of supersymmetric species oscillation. The classic solutions with time-like supersymmetry So far we have considered rather simple classes of BPS configurations and, as we will see, more complex BPS backgrounds can lead to mixtures of both types of supersymmetry. Specifically we want to consider backgrounds that have become the standard fare for the construction of microstate geometries.2 The eleven-dimensional metric has the form: ds121 = (Z0Z1Z2) 3 (dt + k)2 + (Z0Z1Z2) 3 ds42 + (Z0Z2Z12) 13 (dx52 + dx62) 2 1 where the four-dimensional space-time metric has the standard Gibbons-Hawking (GH) form: ds42 = V 1 (d + A)2 + V d~y d~y , The eleven-dimensional Maxwell three-form potential is given by with the five-dimensional Maxwell fields, A(I), given by: A(I) = ZI1 (dt + k) + LI = `I0 + j=1 rj j=1 rj KI = k0I + M = m0 + j=1 rj where rj |~y ~y(j)|. The electrostatic potentials and warp factor functions, ZI , are given by ZI = CIJK V 1 KJ KK 2 V (KI ~LI LI ~KI ) . 2For later convenience we are going to label the species of M2 branes and the corresponding fields by 0, 1, 2 and not use the more usual labeling, 1, 2, 3. We have therefore taken the standard description and replaced the label 3 by 0 everywhere. Merging the two classes of supersymmetry One can uplift the five-dimensional supergravity solutions to six dimensions by using one of the vector fields to make a KK fiber. We will discuss this extensively in section 5 but here we simply want to note that in the six-dimensional uplift there is only one kind of supersymmetry [22, 23]: the null supersymmetry with = 0. The two types of supersymmetry in five dimensions must therefore emerge from the details of the compactification to five dimensions. In this sense one might naturally expect to unify the two classes of supersymmetry, and we will now elucidate how this can be seen directly from the five-dimensional perspective. As have been extensively noted elsewhere [1721] the metric on the four-dimensional base is allowed to be ambi-polar, that is, it is allowed to change signature from (+, +, +, +) to (, , , ). In spite of this, the five-dimensional and eleven-dimensional metrics are smooth and Lorentzian. In particular, this means that V is allowed to change sign and the surfaces where V = 0 are called critical surfaces. One can make a careful examination of the metric (2.6) and Maxwell fields (2.10) and show that the apparently singular terms involving negative powers of V actually cancel out on critical surfaces, leaving a smooth background. It is also important to note that the functions ZI V must satisfy = (Z0Z1Z2) 32 = ((Z0V )(Z1V )(Z2V )) 32 V 2 . Since the ZI V are globally positive, this means that K is time-like except on critical surfaces, where it becomes null. Thus the supersymmetries are time-like almost everywhere, except on critical surfaces where they momentarily become null. It is therefore possible, in principle, to have both types of supersymmetry within one class of solutions. Indeed, black-hole microstate geometries have the same time-like supersymmetries at infinity as a black hole and generically have critical surfaces in the interior of the solution where the supersymmetries become null. It is instructive to see how this comes about in detail. Introduce the obvious frames for the five-dimensional metric: e0 Z1 (dt + k) , e1 (ZV ) 21 V 1 (d + A) , ea+1 (ZV ) 21 dya , Note that we have chosen to write these quantities in terms of the positive functions, ZI V , so that the fractional powers are unambiguous and have no branch cuts. Also observe that the frames e0 and e1 are, respectively, degenerate or singular on critical surfaces. Define null frames: ds52 = (e0)2 + It is also convenient to introduce the quantity Q Z0Z1Z2V V CIJK LI LJ LK + CIJK CIMN LJ LK KM KN . In particular, it follows from (2.25) that Q is smooth across the critical (V = 0) surfaces. The whole point is that while the frames e0 and e1 are singular on the critical surfaces, e+ and e are smooth on these surfaces. To see this, note that e = (ZV )1(dt + ) + (ZV )1 It follows from (2.13) and (2.15) that ZV and V 2 are well behaved on critical surfaces and thus e+ is manifestly well behaved. Now observe that Q = K = (K0K1K2) 13 and note that global positivity of ZI V implies that K0K1K2 > 0 on critical surfaces and so K is real and smooth across these surfaces. As V 0, one finds e K2(dt + ) + 12 K5 Q (d + A) , which are clearly regular as V 0. Finally, define new canonical Lorentzian frames via = 0 = 0 = Z1 = (ZV )1 V , where we are using frame indices based on (2.19). This implies that in this singular frame basis the magnitude of vanishes as O(|V |1/2) when V 0. Passing to the non-singular frames (2.32) requires a Lorentz boost that acts on : = exp = 12 = , remain finite. Thus the Killing spinor is time-like everywhere except where V = 0, where it becomes momentarily null. We therefore conclude that if V 6= 0 then the supersymmetry is precisely that of the three-charge M2-brane system, but on the V = 0 surfaces this supersymmetry becomes compatible with the supersymmetry of M5 branes wrapped on the -circle and with momentum charge on that circle. A degenerate limit and a class of null BPS solutions The fact that, despite appearances, the BPS solutions described in section 2.2 are regular across V = 0 surfaces enables one to take this somewhat further and find classes of BPS solutions by taking V 0 everywhere. As one might anticipate from the discussion above, these solutions have null supersymmetry and are sourced primarily by M5 branes and momentum. To take this limit one can rescale V V everywhere in the solutions of section 2.2 and take to zero. The metric (2.6) simplifies to (dx72 + dx82) + (dx92 + dx120) , (dx52 + dx62) where K is defined in (2.29) and Qb is simply Q with V 0: Qb = 2 K3 M 14 (KI LI )2 + 14 CIJK CIMN LJ LK KM KN . The angular momentum vector, , is now determined by the simpler equation 1 ~ ~ = 2 (KI ~LI LI ~KI ) . The electromagnetic fields (2.10) reduce to the purely magnetic forms: A(0) = A(1) = A(2) = K0 L0 K1 L1 K2 L2 d + ~(0) d~y , K1 L1 K2 L2 K0 L0 d + ~(1) d~y , K2 L2 K1 L1 K0 L0 d + ~(2) d~y . This is the solution that corresponds to the infinite magnetube and, as expected, the Killing vector, = t , is manifestly null everywhere in the metric (2.37). Supergravity coupled to four vector multiplets The supergravity action Species oscillation requires the addition of extra vector multiplets to the N = 2 supergravity theory employed in section 2 and we will therefore summarize the relevant aspects of these theories. Our conventions and normalizations will be those of [24, 25]. The action of N = 2, five-dimensional supergravity coupled to N U(1) gauge fields is given by: S = 1 Z CIJK XI XJ XK = 1 . It is also convenient to define Using the constraint (3.5), one can show that the inverse, QIJ , of QIJ is given by: CIJK = II0 JJ0 KK0 CI0J0K0 . QIJ = 2 XI XJ 6 CIJK XK , and one can show that 1 CIJK XI XJ XK = 1 . (3.8) 6 27 We are simply going to follow [8, 28] and consider eleven-dimensional supergravity reduced on a T 6. The Maxwell fields descend from the tensor gauge field, C(3), via harmonic 2-forms on T 6. The structure constants CIJK are then simply given by the intersection form of the dual homology cycles and the XI are moduli of the T 6. The supersymmetry conditions We start with the most general stationary five-dimensional metric: ds52 = Z2 (dt + k)2 + Z ds42 , where Z is simply a convenient warp factor. Supersymmetry implies, via the condition (2.3), that the metric ds24 on the spatial base manifold, B, must be hyper-Kahler. One now defines N + 1 independent functions, ZI by and then (3.8) implies ZI = 3 Z XI , Z = 1 CIJK ZI ZJ ZK . (3.11) 6 It is more convenient to think of the solution as parametrized by the N + 1 independent scalars, ZI , and that the warp factor is determined by (3.11). Supersymmetry requires that the Maxwell potentials all have the form where B(I) are purely magnetic components on the spatial base manifold, B. One defines the magnetic field strengths accordingly: Having made all these definitions, the BPS equations take on their canonical linear form [29]: where ?4 is the Hodge dual in the four-dimensional base metric ds24, and (24) is the (fourdimensional) Laplacian of this metric. We are, once again, going to take the metric on B to be a GH metric (2.7) and so we will also decompose the vector k according to (2.14). The GH metric and the magnetic fluxes will also be as before and thus we will take V and KI to have the form (2.11). However, we will allow the rest of the solution (ZI , and ~) to depend upon all four variables, (, ~y). The ZI s will still have the form (2.13) but now the LI are general harmonic functions on the base B: (24)LI = 0 . (3.17) The BPS solutions in these circumstances have been discussed in [16, 30]. The last BPS equation, (3.16), can be written as 3 (D~ V V D~ ) + D~ ~ + V ~ = V X ZI ~ V 1KI , This BPS equation, (3.16), has a gauge invariance: k k + df which translates to The four-dimensional Laplacian can be written as (24)F = V 1 V 2 2F + D~ D~ F . (24)LI = (24)M = 0 . If one takes the covariant divergence of (3.18) (using D~ ) and uses the Lorentz gauge choice, one obtains This equation is still solved by D~ ~ + V ~ = V D~ M M D~ V + 2 I=1 1 N+1 KI D~ LI LI D~ KI . One can verify that the covariant divergence (using D~ ) generates an identity that is trivially satisfied as a consequence of (2.8), (3.21), (3.24) and Adding species on the T 4 From the eleven-dimensional perspective, we are going to add extra Maxwell fields coming from three-form potentials with two legs on the T 4 defined by (x5, x6, x7, x8) but leave the fields on the other T 2, defined by (x9, x10) unchanged and supporting only one Maxwell field, which we have labelled as A(0). Thus the only non-zero components of intersection product, CIJK , are for some matrix, CbJK = CbJK . One can easily see that (3.5) implies that, as matrices, Cb3 = Cb and so, assuming that Cb is invertible, we have C0JK = CbJK = CbKJ , The four-torus, T 4, has six independent harmonic forms and by generalizing the Ansatz (2.9) these forms can give rise to six vector fields in five dimensions. However, some of these vector fields belong to N = 2 gravitino multiplets and do not lie in an N = 2 supergravity theory coupled to vector multiplets. Indeed, the vector fields in such an N = 2 supergravity theory are associated with forms in H(1,1)(T 4, C) [8, 26, 27] for a suitably chosen complex structure. We will take this complex structure to be defined by w1 = x5 + ix6 , w2 = x7 + ix8 , w0 = x9 + ix10 . give rise to the other two vector fields, (apart from A(0)), in (2.9). There are two more forms in H(1,1)(T 4, C): 1 1 (dw1 dw2 + dw1 dw2) = (dx5 dx7 + dx6 dx8) , 3 2 2 2 i 1 (dw1 dw2 dw1 dw2) = (dx5 dx8 dx6 dx7) . 4 2 2 2 This leads to an intersection matrix 0 0 0 1 which satisfies (3.28). Indeed the normalizations in (3.31) are set so as to satisfy (3.5) and (3.28) and yield canonical and uniform normalization of the Maxwell fields. The eleven-dimensional three-form potential has therefore the form: C(3) = A(0) dx9 dx10 + This is a very modest generalization of the class of theories considered in [8, 28]. Indeed, we can easily truncate down to A(0), A(1), A(2), A(4) by imposing invariance under the discrete inversion (t, , ~y, x5, x7, x9) (t, , ~y, x5, x7, x9). Observe that (3.11) now implies that the space-time metric warp factor, Z, is given by Z3 = 1 2 Z0 CbIJ ZI ZJ = Z0 It is also convenient to define the quadratic combination: P CbIJ ZI ZJ = The eleven-dimensional metric in this truncation is given by ds121 = Z2(dt + k)2 + Z ds42 + Z Z01 |dw0|2 + P 1 Z2 |dw1|2 + P 1 Z1 |dw2|2 Solutions in six and ten dimensions We are ultimately seeking microstate geometries with species oscillation. This is most easily achieved by using charge density modes on supertubes and for such geometries to be smooth we must go to six-dimensional supergravity. Indeed, one must choose one of the vector fields to become the geometric KK fiber and the remaining N vector fields become encoded in one self-dual and N 1 anti-self-dual tensor multiplets in the six-dimensional theory. We will not need all the details in six dimensions because the smooth Maxwell fields in five dimensions will become smooth tensor gauge fields in six dimensions. The only detail we have to worry about is the singular Maxwell field coming from the supertube source in five dimensions and how this becomes smooth geometry in six dimensions. Lifting to six dimensions The six-dimensional metric is 1 ds62 = 2H1(dv + ) du + k 2 Z0 (dv + ) H ds42 where the four-dimensional base is exactly that of the five-dimensional theory. The functions Z0 and K0 define the geometric KK vector field and so the vector potential, , in (4.1) is V (d + A) + ~ d~y , The six-dimensional warp factor, H, is defined by the quadratic in (3.35) H P = lim r2 Q = 0 , (4.8) r0 where Q is defined in (2.24) and expressed in simplified form in (2.25). The two conditions, (4.7) and (4.8), guarantee that a supertube smoothly caps off the spatial geometry, up to orbifold singularities [1113]. The ten-dimensional IIB configuration The six-dimensional KK uplift above is most simply related to a T 4 compactification of IIB supergravity. It is relatively easy to see what the corresponding brane configuration is by compactifying and T-dualizing the M2 and M5 configurations described in section 3. If one compactifies on x10 then the M2-branes of species 0 become F1-strings wrapping x9 and all the other M2-branes become D2-branes. The M5-dipole charge of species 0 becomes an NS5-dipole charge wrapping , x5, . . . , x8, where is the GH fiber, while all the other M5-dipole charges become D4-dipole charges. Performing the T-duality on x9 converts the F1-strings and NS5-branes to momentum and KK monopole charges respectively, and all the D2-charges become D3-charges intersecting on a common x9 and wrapping the T 4 defined by (x5, . . . , x8) in exactly the same manner as the original M2charges. Similarly, the D4-dipole charges become D3-dipole charges intersecting on the common -circle and wrapping the T 4 defined by (x5, . . . , x8) in exactly the same manner as the original M5 dipole charges. Thus we obtain a IIB configuration in which all the M2 species have become either D3branes or momentum. One can perform two more T-dualities on the T 4, for example along (x5, x6), thereby converting two of the sets of D3-charges into D1- and D5-charges. This T-duality changes the other D3-charge species into D3-charges with different orientation, and introduces additional NS-NS B-fields on the T 4. Thus one can obtain the canonical D1-D5-P system decorated with additional D3-charges. This last T-duality does not affect the space-time metric and its regularity. There is another way to dualize our configurations to magnetubes with D1 and D5 charges. If one starts from a magnetube whose D1 and D5 charges oscillate into F1 and NS5 charges [1], there is a duality sequence, given by equation (3.1) in [8], that takes this solution into a solution of the type we construct here but where the species corresponding to A3 and Z3 is absent. Hence, if one applies the inverse of this duality sequence on a solution with A3 = 0 = Z3 one obtains the magnetube of [1]. If one applies the inverse duality sequence to a more general solution, where the third species is also present, the resulting magnetube will have two extra charges, corresponding to D3 branes with two legs along the T 4 and one along the common D1-D5 circle. The non-oscillating template We now describe in detail a simple example of a smooth magnetube geometry, which we will construct by putting a single supertube (with no species oscillation) on the V = 0 surface in the simplest ambipolar Gibbons-Hawking space. The discussion here follows closely previous work on supertubes in such backgrounds, but there is some novelty in dealing with putting the supertube on the V = 0 surface. Our aim in this section is to show that the conditions for smoothness of the supertube are unchanged by placing it on the V = 0 surface, and hence translate directly in the conditions for smoothness of a magnetube. The non-oscillating solution provides a simple context to deal with these issues and set up the framework before we move on to introduce species oscillation. We will see later that for the solutions with species oscillation we can choose the charge densities such that the angular momentum density remains constant, and then the structure of the metric in the oscillating solutio n is almost identical to that of the non-oscillating solution. We start from the simplest solution with a non-trivial critical surface, a two centered metric. We first review the background solution before we introduce the supertube; we consider a particularly simple example in which the five-dimensional geometry is simply AdS3 S2 [1416]. This solution is axisymmetric and so it is more convenient to write the four-dimensional base in terms of cylindrical polars on the flat R3 slices: ds42 = V 1 d + A)2 + V (d2 + dz2 + 2d2) . For simplicity we take the two GH charges to be equal and opposite, so V = rq+ rq , for some parameter a. In this simple two-centered solution, the solution will have the classic form of section 2.2 with two vector multiplets, except we will use the labeling {I, J, K} = {0, 1, 2} instead of the more common usage ({I, J, K} = {1, 2, 3}). We initially take the magnetic flux functions, KI , to have the simple form where r p2 + z2. The electric source functions, LI , are set to 1 r The coefficients of the r1 terms in the LI have been fixed by the usual regularity condition for bubbled geometries in five-dimensions: ZI should be finite at r = 0. The harmonic function M in the angular momentum is Again the coefficients of the r1 terms in M have been fixed by the usual five-dimensional regularity conditions for bubbled geometries: must be finite at r = 0. The parameter m is introduced to ensure smoothness and lack of Dirac strings. Finally, the 3-dimensional angular-momentum vector, , is determined using (2.16): To make sure that there are no CTCs near r = 0 and to remove Dirac strings, we must impose the five-dimensional bubble equations: (r = 0) = 0. For this two-centered solution this requires only that In particular, one has Rescaling and shifting the remaining variables according to the five-dimensional metric then takes the standard global AdS3 S2 form: ds52 R1 cosh2 d 2 + d2 + sinh2 d12 2 R1 = 2R2 = 4k . (5.14) One should note that an observer whose world-line has tangent, u , i.e. the observer is fixed in the GH spatial base, follows a curve with which means that the proper 4-velocity has norm: 4k2 cos2 . Thus this GH-stationary observer follows a time-like curve everywhere except on the equator ( = 2 ) of the S2 where the observers trajectory becomes null. This illustrates the general discussion in section 2.3: in patches that are smooth across the critical surface V = 0, the GH-stationary observers are being boosted from time-like to null trajectories as V 0. Adding the supertube/magnetube k2 L0 = q 1 r 1 r The coefficients of the r1 terms in the LI are as before. The sources at r = 0 in K0, L1 and L2 correspond to those of a supertube with dipole charge and electric charges 1 and 2. We want to demonstrate that for appropriate choices of these parameters the addition of this supertube leads to a smooth six-dimensional geometry that asymptotically approaches an AdS3 (S3/Z2k+) geometry. The harmonic function M in the angular momentum is now Again the coefficients of the r1 terms in M are as before. The parameter m0 represents the angular momentum of the supertube while the parameter m is introduced to ensure smoothness and lack of Dirac strings. Finally, the 3-dimensional angular-momentum vector, , is determined using (2.16) and we now find 2k3 2 + (z a + r+)(z + a r) = qa r+r + a1 m0q + 2kq2 2 + (z arr++r+)(z r) + 2 + (z + rr)r(z + a r) Regularity near sources To make sure that there are no CTCs near r = 0 and to remove Dirac strings, we must impose the five-dimensional bubble equations: (r = 0) = 0. This now imposes two constraints: Since K1 = K2, the absence of Dirac strings at the magnetube is already guaranteed by (5.20). This is, of course, to be expected since a Dirac string must have two ends and we have eliminated them everywhere else. The other supertube regularity condition (4.8) is easily computed from (2.25) particularly since V = 0 and L3 = 0 at r = 0. One finds that this condition is satisfied if which is the standard relationship between the charges and angular momentum of a supertube. The free parameters are then just the charges , , as is standard for a supertube. Geometry of the regular magnetube For the later discussion of the oscillating solution, it is useful to summarize here the functions appearing in the six-dimensional metric (4.1) for the non-oscilating magnetube solution and to note explicitly where the parameter enters into the solution. The KK electric function Z0 is independent of the magnetube parameters, Z0 = V + L0 = V + L, where K, L are given by (5.4) and (5.5). The other electric functions are so the warp factor H is K3 K2 3k2 k2 = V 2 + r V 2 2q2 K 2q2 r + M, where M is given by (5.18) with the parameters fixed by (5.21) and (5.23). Thus, the electric charge parameter, , only enters the metric (4.1) directly through the warp factor, H, and appears indirectly in the one-form k through the dependence of m0 on from (5.23). Of course, will also appear directly in the gauge fields A(1) and A(2). AdS3 S3 asymptotics at infinity One can use the spherical bipolar coordinates (5.9) to study the asymptotic form of our solution. The warp factor H will behave as H To obtain the leading asymptotics, we only need to consider the first term. As , the leading-order behaviour of the metric is 2k(2k + ) d2 + sin2 d22 + One can, in fact, allow equality here but then the metric becomes asymptotic to some form of null wave in which only the d du term survives at infinity. If < 0 then the -circles become closed time-like curves. We assume that (5.32) is true. The leading-order asymptotics of the matter fields can similarly be calculated; the two non-KK scalar fields are X1 = so asymptotically X1 = X2 = 1 + + O(e4). (5.34) 2k The background value of the scalar fields is rescaled along with the AdS3 radius of curvature, and there is no sub-leading part at order e2, so there is no vev for the dual operators. The two non-KK vector fields are 2 4 q k2(2k + ) + 2 k2 (a2kq + ) u KI A(I) = ZI1(dt + k) + (d + A) + ~(I) d~y , I = 1, 2 , so we get the same component on the sphere, consistent with the fact that the spheres radius of curvature is unchanged in the metric (5.29). The second term is locally pure gauge, but as is a compact direction it introduces a Wilson line. In AdS3, the asymptotic behavior of a massless gauge field is A A(0) + j ln r, where A(0) is interpreted as the boundary gauge field and j is the vev of the boundary conserved current. The absence of a logarithmic term in r (a linear term in ) in the expansion (5.36) thus indicates that the introduction of the magnetube does not produce any charge density from the point of view of the dual CFT; the only effect of is to turn on a Wilson line along the circle. Global regularity As we remarked earlier, the two conditions (4.7) and (4.8) guarantee that a supertube smoothly caps off the spatial geometry [1113] and so, in principle, (5.20), (5.21) and (5.23) guarantee that the supertube is smooth in six dimensions. However, we actually have a magnetube: that is, a supertube located at the critical (V = 0) surface. While this should not affect the arguments of [12, 13], we will now examine the metric in more detail to confirm that the magnetube limit of the supertube does not add any further subtleties. Even though the metric appears to be singular at the critical surfaces (V = 0), it is well known that it is actually smooth across such surfaces (see, for example, [20]). There is also an apparent singularity at r = 0 but this is resolved by the standard change of coordinate that shows that the supertube is smooth in six dimensions [1113]. In the solutions we are considering, these two apparent singularities coincide and while the methods of resolution of the two types of apparent singularity are not expected to interfere with each other, it is important to make sure. Expanding (4.2) in spherical polar coordinates around r = 0, one obtains the leading order behavior: 1 (2k + ) k2 2 + (2k ) q2 2 . Provided that Q0 > 0, the metric (5.37) is manifestly a time and S1 fibration defined by (u, 1) over a four-dimensional spatial base defined by (r, , 2, v). The apparent singularity at r = 0 in this spatial base is resolved in the usual manner by changing to a new coordinate, R, defined by r = 14 R2. Thus this spatial base is an orbifold of R4, and the whole metric is smooth up to such orbifold singularities. Indeed if one restricts to slices of constant (u, 1), then one has d = 21q d and the four dimensional base metric becomes ds42 2ka dR2 + 14 R2 d2 + sin2 If one remembers that has period 4 then one sees that this is precisely the metric of flat R4 for q = = 1. Other integer values of and q thus lead to orbifold singularities. Smoothness around r = 0 this requires Q0 > 0. If 2k > then this is manifest, but if not one can use (5.32) to replace 2 and conclude that 4 k4 32 k6 Q0 > q2 a3 (2k + ) + (2k ) (4k + ) = q2 a3 , which establishes positivity. Global regularity of the solution also requires that the functions HV , Z1Z21 and Z0H1 are globally positive and well-behaved, except for possible singularities allowed by supertubes. In particular, this means that all the functions ZI V must be globally positive. This is trivial to see for Z0V since it may be explicitly written as Z0 V = r+ r 4k2 r + k (r+ + r) q (r+ r) 4k2 r + k (r+ + r) |q (r+ r)| 4k2 r + k (r+ + r) k (2k + ) | (r+ r)| . where we have used the fact that (5.32) implies |q | < k(2k + ). Suppose (r+ r) > 0, then we may write this as 2 k2 (r + r a) + 2 k2 (r + a r+) + 2 k r 0 , Similarly one can write ZI V = 1 r r+ r 1 r r+ r 1 > r r+ r g t t = gtt = ((Z0V )(Z1V )(Z2V ))1/3(Q 2) > 0 , where is squared using the R3 metric. Thus we need to verify the global positivity of (Q 2). For large values of r, one finds where is defined by (5.31) and hence (5.32) guarantees that (Q2) is positive as one goes to infinity. Beyond this, we have examined this quantity in several examples of solutions satisfying (5.32) and found them to be stably causal. A typical example is shown in figure 1. Species oscillation Our primary contention in this paper is that species oscillation can be done on any V = 0 surface in any microstate geometry based upon a generic GH base. However, the essential Greens functions for such generic microstate geometries are not explicitly known. On the other hand, the introduction of species oscillation involves a localized source and the twocentered solution considered in section 5 provides an excellent local model of a typical V = 0 surface in a generic microstate geometry. Moreover, the Greens functions for this relatively simple system are known [16] and so the solutions can be constructed explicitly. Given that species oscillation can be implemented, in a very straightforward manner, to produce new classes of microstate geometries within such a local model, we believe that the generalization to any microstate geometry should present no difficultly apart from the fact that explicit analytic examples may not be available. Some simple oscillating solutions We will thus construct the simplest example of a non-trivial solution with species oscillation: we add a magnetube with an oscillating charge distribution to the simple two-centre background from the previous section. The first step will be to allow the electric charge sources in (5.17) to be -dependent much as in [16], however here these charges will oscillate into other species of M2-brane charge. To enable this species oscillation we add two vector multiplets as discussed in section 3 but only give allow them to have electric charges. We therefore take the GH base with V still given by (5.2) and keep the same magnetic sources as in (5.16): K3 = K4 = 0 . The electric source functions, LI , are set to: k2 L0 = q 1 r I = 3, 4 , for some charge-density functions, I (). As before, this corresponds to a supertube that wraps around the circle and now carries four kinds of electric charges, I (), as well as the magnetic dipole charge . We will assume that the integral over of the chargedensity functions I () vanishes, so that (as we will show later for the asymptotic charges) the supertube is carrying no net electric charge; the electric charge oscillates between the different species as we go around the circle. This is the key difference from previous studies with varying charge density [16], and is possible because we take the supertube on the V = 0 surface. Since K3 = K4 0, it follows that It was shown in [16] that for the -dependent solutions we are considering here, supertube regularity can be analyzed locally in and that regularity is, once again, ensured by imposing (4.7) and (4.8). As before, (4.7) guarantees the absence of Dirac strings and, equivalently, this relevant condition can be obtained from (3.25) by requiring that ~ has no sources of the form of a constant multiple of ~ 1r . Using the fact that K1 K2, K3 = K4 0 and V and L0 vanish at r = 0, this Dirac string condition implies that the singularities in L1 and L2 must be equal and opposite at r = 0 and thus: This equation is the generalization of (5.20) to a magnetube with species oscillations. On the other hand, one can also recover this equation by starting from a supertube that is not Using (6.9) and K1 K2, K3 = K4 0 and the vanishing of V and L0 at r = 0, the second regularity condition collapses in the relatively simple condition: This implies that 2 () = 1() 2() 12 (3()2 + 42()) = 1()2 + which is the analog of (5.23). A similar relation between () and the other charge densities was also found in [16]. Note that while the integral of I () vanishes, the integral of () cannot (for non-trivial charge densities) and so the supertube will carry a net angular momentum. A regular supertube is then parametrized by the constant dipolar magnetic charge and three independent electric charge densities, 1(), 3() and 4(). For general charge densities, the example constructed above will have a metric that is a nontrivial function of , although it will become -independent asymptotically. Remarkably, however, we can choose the oscillating charge densities in such a way that the metric is completely independent of . As described in the Introduction, this works in a manner rather reminiscent of Q-balls: the species fluctuate but the energy-momentum tensor, and hence the metric does not. The basic idea is to arrange that 1(, ~y)2 + 1 3(, ~y)2 + 4(, ~y)2 = (~y)2 , 2 for some function (~y). From the asymptotic properties of the I , it follows that we must have as this must be satisfied for all ~y, and we only have the freedom to choose the source functions that are functions only of . However, the isometry of the base metric along means that the solution can be decomposed into Fourier modes, and if we take the source charge densities to involve a single Fourier mode, then we can take solutions I (, ~y) that take a product form, I (, ~y) = Fn(~y)I (), and the ~y dependence factors out of (6.12) which reduces simply to (6.13).3 Thus, we can satisfy (6.12) by taking, for example, where is a constant and Fn is normalized so that Fn 1r as r |~y| 0. In this way, species 1 is locked to species 2 and they oscillate into species 3 and 4. (There is obviously a family of choices of how to distribute the oscillations amongst species 3 and 4 in such a way as to satisfy (6.13).) We will compute the details of the functions Fn in section 7, but before going into the technicalities we can make some observations about the solution. First note that (6.13) and (6.11) imply that () is constant, and the identity (6.11) collapses precisely to that of the template solution (5.23). This means that the function M is exactly as in (5.18). Note, in particular, that M still knows about the amplitude, , of the species oscillation. Furthermore, having K1 K2, K3 = K4 0 and 1 = 2 means that the I cancel out in the function in (2.15) and so it is exactly the same function as it was in the template solution of section 5. Similarly, the I cancel out in (3.25) and the fact that M is independent of means that satisfies exactly the same equation as in the template solution and so is identical with the solution (5.19). The only difference between the metric of the oscillating solution and the metric of the template arises in the warp factor, H, given by (4.5). It follows from (2.13), (6.1), (6.2), (6.5) and (6.12) that H2 = The important point is that this function is independent of and thus is still a Killing vector of the metric even though the Maxwell fields and scalars are -dependent. Because of (6.13) the function H also has exactly the same behavior as r 0 as its counterpart (5.26) in the template solution. Thus the local regularity of the metric is guaranteed by that of the template solution. The fact that the metric is unchanged apart from this change in the warp factor H also implies that leading-order asymptotics of the metric are also the same as for the nonoscillating solution. Indeed, the asymptotics is independent of the assumption that the full metric is -independent. Any -dependence in H is subleading at large distances, and thus so long as (6.13) is satisfied so that the angular momentum is -independent, the leading-order asymptotics will be the same as in the non-oscillating solution. Thus, for all solutions satisfying (6.13), the overall amplitude of the oscillating charge densities is bounded by (5.32). Furthermore, the (~y)2 in (6.15) will not contribute to the asymptotic stress tensor: as we we will see in the next subsection, the functions Fn(~y) represent higher multipole moments and therefore fall off faster than 1/r, so (~y)2 in (6.15) falls off faster than 1/r2. Thus this term falls off too fast to contribute to the sub-leading part of the metric that gives the asymptotic charges. For the gauge fields, there was no contribution to charges in the non-oscillating case due to the absence of a logarithmic term in (5.36); the faster fall-off in the oscillating solution does not change this. Thus, the asymptotics of solutions with species oscillation where the angular momentum density is a constant is very similar to the non-oscillating case. The only notable difference in the asymptotics is that the suppression of Fn(~y) implies that the Wilson line noted in (5.36) is absent in the oscillating solution. The oscillating modes The Greens function To obtain the explicit details of our oscillating solution we need to solve (3.17) on the base defined by (2.7) with (5.2). Fortunately the relevant Greens function was computed in [16]. The expression for this function was very complicated but here there are significant simplifications because we have put the source point, (0, ~y), at ~y = 0. Define the following combinations of coordinates: (2 u2 1 + y2) p1 y2 p(2 u2 1)2 y2 , Thus the end result can be expressed as a rational function of these variables. In particular, it is useful to note that p(2 u2 1)2 y2 = The Greens function can then be written as [16] Gb = a u1 y Re w(1 y w) 1 (w w+)(w w) pu2 y w 1 w = 2 a u y (w w+)(w w) where we have used the fact that w = w1. There are several important things to note: (i) r = 0 corresponds to u = 1 and y = 1 and we are going to work in the region r > 0 in which y1u2 > 1. (ii) The branch points of pu2 y w are at infinity and at w = y1u2 > 1 and since |w| = 1, the branch cuts can be arranged to be safely outside the unit circle. (iii) The fact that w+w = 1 means that one of the poles at w is outside the unit circle while the other is inside. We are choosing signs of square roots so that |w| 1 |w+|. (iv) The poles at w coincide at 1 if and only if y = 1. This is the critical surface, and a careful examination of (7.7) shows that Gb = 0 when y = 1 and is indeed well-behaved across this surface. The Fourier modes The explicit modes One can obtain the Fourier modes from this Greens function by integrating against ein( 21q 00) = wnein( 21q ). Dropping the phase factors of ein( 21q ), the functions of where the contour is taken counterclockwise around the unit circle and 1 I |w|=1 w dw wn F (w) + F (w1) , Since F (w1) has a branch cut inside the unit circle, we make the inversion, w w1 in this integral (remembering that the inversion also inverts the orientation of the contour) and write it as 1 I |w|=1 w dw (wn + wn) F (w) . Note that for n = 0 this simply gives r1 and this has been used to set the normalization of Fn in general. For general n we can write this in terms of Chebyshev polynomials: pu2 y w = Fn(w) = (w+n + wn) . where Tn is the nth Chebyshev polynomial of the first kind and x is given by (7.3). where Up(x) are Chebyshev polynomials of the second kind. This series converges for |w| < |w| and hence near w = 0. The residue at w = 0 can then be written as 1 uy2 w Thus the solutions to (6.3) can be written as linear combinations of the modes: Fn ein( 21q ) = Fn(0) + Fn(w) ein( 21q ) . with Fn(0) and Fn(w) given by (7.15) and (7.13). In particular, Fn(w) gives rise to the singular source at r = 0 and the remaining parts are essential corrections as we now discuss. On-axis limit As we have already seen, |w|=1 w dw (wn + wn) = a (2u12 1) n,0 . and this was used to set the normalization of the modes. The first few Chebyshev polynomials are T0 = 1 , T1 = x , T2 = 2x2 1 ; U0 = 1 , U1 = 2x , U2 = 4x2 1 . F0 = F1 = r+ + r 2r F1 F2 where we have used (7.4) and (7.5). Similarly, one has F2 = 4(2r a) 6 (r+ + r + 2a)2 + (r+ + r + 2a) Note that both F1 and F2 vanish on the axis, where r+ + r = 2r. Moreover they both have a canonically normalized source at r = 0: Asymptotics of the modes at infinity From the explicit examples above one sees that the modes Fn 1/rn+1 as would be expected from charge multipoles. We can easily prove this form in general by recalling that the Greens function (7.7) was obtained in [16] by taking the Greens function on the AdS3 S2 space (5.12) and Kaluza-Klein reducing to obtain the Greens function on the ambi-polar base. The asymptotic behaviour of the Fourier modes of the Greens function on the AdS3 S2 space is then easily obtained by a conventional spherical harmonic analysis on the S2. From the perspective of AdS3 S2, since 2 = 21q + 2 , our Fourier expansion G = Pn Fn(u, y)wn corresponds to an expansion The Greens function can be decomposed in terms of the spherical harmonics Ylm(, 2) on the S2; in this decomposition, Fn will only involve spherical harmonics with l n. Doing a Kaluza-Klein reduction on the S2, the massless wave equation on AdS3 S2 becomes a massive wave equation on AdS3 for each spherical harmonic mode with a mass m2 = l(l + 1)/R22 = 4l(l + 1)/R12. Thus, Fn = Pl>n Fln where at large sinh 21 sinh 2Fln 4l(l + 1)Fln, so Fln e2(l+1), that is at most Fn 1/rn+1. From the perspective of the AdS3 S2 asymptotics, the species oscillation of the supertube is introducing a variation of the fields along the 2 direction in the S2, so it corresponds to exciting higher KK harmonics, which produce vevs for higher-dimension operators in the dual CFT rather than exciting local charge densities of the conserved currents. Comments on supersymmetric species oscillation Our aim has been to show that the object underlying the species oscillation idea introduced in [1] is a supersymmetric magnetube: a combination of (M5 and P) magnetic charges as well as several oscillating (M2) electric charges, that carries the same supersymmetries as M5 branes and momentum regardless of the oscillations of its electric charges. Trying to bend this object into a ring in R4 will break these supersymmetries, and will result in neutral configurations that have been proposed in [1] to describe microstate geometries of neutral Schwarzschild black holes. We have also succeeded in realizing the species oscillation idea in a supersymmetric context, by embedding the magnetube into supersymmetric solutions. In doing this we have uncovered a remarkable unification of the timelike and null types of supersymmetries directly in the framework of five-dimensional supergravity; the timelike supersymmetry on an ambi-polar background becomes locally null on the surface V = 0. Hence an object that would be invariant only under the magnetic-type null supersymmetries, like the magnetube, can be placed on this surface while preserving the global electric-type timelike supersymmetry. This enables us to construct solutions with species oscillation which preserve supersymmetry globally. We have carefully analyzed the smoothness conditions for magnetubes on the V = 0 surface, initially for a magnetube without species oscillation and then for a magnetube with M2 electric charge densities that vary around the tube in such a way that the net M2 charges vanish. We found that this magnetube can be obtained by moving a supertube onto the V = 0 surface (which corresponds to giving it an infinite boost) and that, in the V 0 limit, the smoothness conditions of the supertube are enough to ensure the smoothness of the magnetube. We constructed a simple example of a solution with species oscillation and gave an explicit description of its structure. In this example, the geometry is independent of the coordinate; the gauge fields are oscillating but their combination in the stress tensor is -independent, as in the exact near-tube solution discussed in [1]. The simple example we have considered is asymptotically AdS3 S2, and it would be interesting to understand the interpretation of the solution with species oscillation from the point of view of the dual CFT. A key aspect is that when we introduce the -dependent source, the non-diagonality of the metric in the angular coordinates makes the solution a function of 2q , as can be seen in the Greens function (7.6). This combination becomes an angle in the S2 factor in the asymptotic solution (5.12). Thus, from the point of view of the AdS3 S2 background, the species oscillation is not introducing dependence on the angular coordinate in the AdS3 (shifting 1 at fixed 2 remains a symmetry of the solution) but on one of the angular coordinates on the S2. Thus, understanding the interpretation of our solution in the dual CFT will involve a Kaluza-Klein decomposition along the lines of [31]. It will obviously be interesting to further exploit this new freedom in constructing supersymmetric smooth microstate geometries. It gives us a new possibility to introduce dipole charges. Examples of solutions with varying charge densities were previously constructed in [16], but we can now construct solutions with zero net charge. Another interesting direction for further development is to consider species oscillation on supersymmetric black strings and black rings. Non-BPS, asymptotically flat solutions Following the direction of [1], probably the most interesting question to ask is if one can deform our supersymmetric solutions to construct non-supersymmetric asymptotically-flat solutions, as a step towards constructing microstates for black holes like Schwarzschild. The solution we constructed above is asymptotically AdS3 S2, but one should be able to construct similar supersymmetric solutions that are asymptotically flat in five dimensions by considering a supertube/magnetube at the V = 0 surface in a more general GibbonsHawking base that gives rise to an asymptotically flat background. We have also seen that the oscillating charge distributions do indeed make no net contribution to the charges measured from infinity. On the other hand, the size of the oscillation is still bounded by the background magnetic fluxes and hence by the asymptotic charges. It is remarkable that one can have stationary asymptotically flat solutions; one might physically expect that a varying charge density on a rotating object would give rise to time-dependent multipole moments, which would lead to electromagnetic radiation. However, the resolution is a familiar effect in supertubes; the supertube is rotating, but the charge on the supertube corresponds to a charge density wave traveling around the tube in the opposite direction, so that we get a standing wave. As a result, the multipole moments of our supersymmetric solutions, whose oscillating parts may be viewed as superubes/magnetubes, will all be time-independent. On the other hand, this cancellation of the time-dependence coming from having a standing wave is a fine-tuned phenomenon. If we excite the supertube/magnetube by adding some energy, we will need to make it rotate faster to maintain the stabilization by angular momentum, and it is possible that the counter-rotating charge density wave will then give rise to time-dependent multipole moments. If true, this would a real obstacle to finding stationary non-supersymmetric solutions. Note also that the non-stationarity is associated with the emission of electromagnetic radiation, so the natural timescale for the decay is likely to be much faster than the gravitational timescales associated with a black hole. The solution discussed in [1] is vulnerable to a similar problem. In the exact near-tube solutions the authors introduce dependence on a null coordinate t a, corresponding to a charge density that is a function of t a. In the near-tube solution is a coordinate along a straight black string, and this is related to a solution with charge density depending just on the position along the string by an (infinite) boost. But in the full asymptotically-flat solution this corresponds to a truly time-dependent charge distribution, and we expect that this will lead to electromagnetic radiation in the sub-leading corrections to the solution, introducing time-dependence in the metric on a timescale set by the electromagnetic radiation reaction. Thus we believe that species oscillation has opened up an even larger, new moduli space of BPS microstate geometries but remain uncertain whether this idea can be adapted to yield stationary non-BPS configurations. Acknowledgments We would like to thank Samir Mathur and David Turton for extensive discussions and for providing us with an advance copy of [1]. We would also like to thank Stefano Giusto, Rodolfo Russo and Masaki Shigemori for useful discussions. NPW is grateful to the IPhT, CEA-Saclay and to the Institut des Hautes Etudes Scientifiques (IHES), Bures-sur-Yvette, for hospitality while this work was done. NPW would also like to thank the Simons Foundation for their support through a Simons Fellowship in Theoretical Physics. SFR would like to thank the UPMC for hospitality while this work was done. NPW and SFR are also grateful to CERN for hospitality while this work was initiated, and we are all grateful to the Centro de Ciencias de Benasque for hospitality at the Gravity- New perspectives from strings and higher dimensions workshop. The work of IB was supported in part by the ANR grant 08-JCJC-0001-0, and by the ERC Starting Independent Researcher Grant 240210String-QCD-BH and by a grant from the Foundational Questions Institute (FQXi) Fund, a donor advised fund of the Silicon Valley Community Foundation on the basis of proposal FQXi-RFP3-1321 to the Foundational Questions Institute. This grant was administered by Theiss Research. The work of NPW was supported in part by the DOE grant DE-FG0384ER-40168. SFR was supported in part by STFC and the Institut Lagrange de Paris. Open Access. This article is distributed under the terms of the Creative Commons Attribution License (CC-BY 4.0), which permits any use, distribution and reproduction in any medium, provided the original author(s) and source are credited.


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Iosif Bena, Simon F. Ross, Nicholas P. Warner. On the oscillation of species, Journal of High Energy Physics, 2014, 113, DOI: 10.1007/JHEP09(2014)113