On Classical Stability with Broken Supersymmetry

We study the perturbative stability of four settings that arise in String Theory, when dilaton potentials accompany the breaking of Supersymmetry, in the USp(32) and U(32) orientifold models, and also in the heterotic SO(16)xSO(16) model. The first two settings are a family of AdS3xS7 orientifold vacua and a family of AdS7xS3 heterotic vacua, supported by form fluxes, with small world-sheet and string-loop corrections within wide ranges of parameters. In both cases we find some unstable scalar perturbations, as a result of mixings induced by fluxes, confirming for the first class of vacua a previous result. However, in the second class they only affect the l=1 modes, so that a Z2 projection induced by an overall internal parity suffices to eliminate them, leading to perturbative stability. Moreover, the constant dilaton profiles of these vacua allow one to extend the analysis to generic potentials, thus exploring the possible effects of higher-order corrections, and we exhibit wide nearby regions of perturbative stability. The solutions in the third setting have nine-dimensional Poincare' symmetry. They include regions with large world-sheet or string-loop corrections, but we show that these vacua have no perturbative instabilities. Finally, the last setting concerns cosmological solutions in ten dimensions where the"climbing"phenomenon takes place: they have bounded string-loop corrections but large world-sheet ones close to the initial singularity. We find that perturbations generally decay, but homogeneous tensor modes exhibit an interesting logarithmic growth that signals a breakdown of isotropy. If the Universe then proceeds to lower dimensions, milder potentials from other branes force all perturbations to remain bounded.


Introduction
When Supersymmetry is broken in String Theory [1], one is inevitably confronted with stability issues. These are particularly severe when tachyons emerge, but even in the few cases when this does not occur runaway dilaton potentials destabilize the original ten-dimensional Minkowski vacua. Supergravity [2] is the key tool to analyze these systems, within its limits of applicability.
There are three ten-dimensional string models with broken Supersymmetry and no tachyons, and two of them are orientifolds [3] of closed-string models. The first of these is the U Sp (32) model [4] with "Brane Supersymmetry Breaking" (BSB) [5], a peculiar type-IIB orientifold which combines the presence of a gravitino in the low-energy Supergravity with a non-linearly realized Supersymmetry [6]. The second has no Supersymmetry at all, and is the U (32) 0 B model [7], a non-tachyonic orientifold of the tachyonic 0B model [8]. In both cases, an exponential dilaton potential emerges at the (projective-)disk level, which reflects the residual tension of the branes and orientifolds that are present in ten dimensions. In the Einstein frame it reads There is finally a heterotic model of this type [9], with an SO(16) × SO (16) gauge group. Its torus amplitude gives a contribution that in the string frame is independent of the dilaton, but in the Einstein frame this translates into the dilaton potential [10] V = T e In the first case there is a class of AdS 3 ×S 7 vacua [11], which are sustained by three-form (electric) fluxes that permeate AdS 3 , and where the dilaton has constant profiles. In the second case similar steps lead to a class of AdS 7 × S 3 vacua [11], which are sustained by three-form (magnetic) fluxes that permeate the internal S 3 , and where the dilaton has again constant profiles 1 . In both cases there are wide corners of parameter space where large radii and small string couplings are possible.
In this paper we investigate perturbative stability in the presence of broken Supersymmetry in four types of settings. The first two concern these AdS vacua for the orientifold and heterotic models, where fluxes counteract the effects of gravity. The third concerns the Dudas-Mourad solutions with nine-dimensional Poincaré symmetry [12], the first that were found for the low- with nine-dimensional Euclidean symmetry, which were also first found in [12] and where the string coupling has an upper bound, so that string corrections are in principle under control, while curvature corrections are still large close to the initial singularity. Some generalizations of this solution were found later in [15], and were elaborated upon in detail in [16], where they were associated to the picture of a "climbing scalar". Amusingly, the orientifold potential in eqs. (1.1) corresponds indeed to a "critical" logarithmic slope where the scalar (the dilaton in ten dimensions or, in lower dimensions, a mixing of it with the breathing mode of the internal space [17]) becomes compelled to climb up the potential when emerging from the initial singularity. In the subsequent descent the potential energy thus collected can give the initial impulse to start inflation [18]. This is the case if milder potentials, which could arise from lower-dimensional branes, are taken into account [19,20]. The generic indication of these scenarios, if a short inflation happened to have left us some glimpses of its inception, resonates with the lack of power displayed by the first CMB multipoles [21]. Our discussion will make these considerations a bit more concrete from a top-down perspective.
There is an extensive activity aimed at identifying and cutting out, within the vacua that arise in Supergravity, wide subsets that should not admit ultraviolet completions, and therefore should not pertain to String Theory proper [22]. There is also a widespread feeling that instabilities show up generically in non-supersymmetric contexts. When this is the case perturbations, even if initially small, grow generically in time, and a pathology of this type is precisely what the negative squared masses of tachyons signal in flat space. In AdS d vacua matters are a bit subtler, and the proper stability conditions, which are called Breitenlohner-Freedman (BF) bounds [23], allow for finite ranges of negative squared masses, in ways that depend on the dimension d and on the nature of the fields. Hence, one can study perturbative stability in AdS backgrounds analyzing the eigenvalues of (properly defined) squared mass matrices for the available modes. This will be a primary task of this paper, and in particular we shall confirm the instability found in [24] for the AdS 3 × S 7 family of vacua, which were actually first considered there, and we shall also present a similar result for the AdS 7 × S 3 heterotic vacua of [11]. The instabilities present in both cases comply with the general expectations in [22], but the relative simplicity of these settings allows us to move further.
In the AdS ×S vacua of [11,24] the dilaton has constant profiles. This makes it possible to scan the behavior of perturbations in a wide class of systems simply modifying three constants, the vacuum value V 0 of the potential and those of its first derivative V 0 and of its second derivative V 0 . One can explore, in this fashion, whether perturbative instabilities are generic within the potentials that give rise to similar AdS × S flux vacua. The lesson that we shall gather is clearcut: close to the actual values, and as soon as V 0 becomes negative, there are wide regions of perturbative stability. This interesting phenomenon occurs both in the AdS 3 × S 7 orientifold vacua and in the AdS 7 ×S 3 heterotic ones, and the nearby regions could play a role when string corrections are taken into account, although we are unable to justify dynamically the emergence of such deformations via quantum corrections. Moreover, in the AdS 7 × S 3 heterotic vacua the instability affects only the = 1 scalar modes, so that it can be eliminated by an antipodal projection in the internal sphere. We also explored similar, albeit more complicated, operations for the orientifold vacua. In particular, in the simpler case of an internal S 3 one could work with unit quaternions, removing all unwanted spherical harmonics with = 2, 3, 4 via projections based on the symmetry group of the cube in R 3 . This would leave no fixed sub-varieties, and therefore constitutes an alternative option for the heterotic case. Its direct counterpart in S 7 , however, appears much more complicated, since it would rest on octonions. We thus explored, as an alternative, a construction based on three quaternion pairs, which does eliminate all unwanted spherical harmonics but unfortunately fixes some sub-varieties.
The following sections deal with the nine-dimensional vacua with Poincaré symmetry and the cosmological solutions that were discovered in [12], and also with the linear-dilaton systems of [13,14] and other generalizations. As we shall see, the nine-dimensional vacua are perturbatively stable solutions of Einstein's equations although, from the vantage point of String Theory, they include regions of high curvature and strong coupling, where corrections to Supergravity are expected to play an important role. Some features of these higher-derivative couplings were explored in [20]. In the spirit of the preceding extensions and in view of their potential applications, we also analyze the cosmological solutions that arise, in lower dimensions, with similar potentials e γ φ , for different values of γ. These potentials were first studied in [15], and this will also connect the present analysis to the work in [16]. The resulting indications are that perturbations are wellbehaved, up to an intriguing behavior of the homogeneous, k = 0 mode that manifests itself, in ten dimensions, with the potentials of eqs. (1.1) and (1.2) in the absence of milder terms, to which we shall return in Section 7.1.
The contents of this paper are as follows. In Section 2 we define the low-energy Lagrangians of interest and we explain our conventions. In Section 3 we review the AdS 3 × S 7 orientifold vacua of [11,24] and extend them in the most general way that is of interest with constant dilaton profiles, allowing for generic values of the potential V 0 , its first derivative V 0 and its second derivative V 0 . In Section 3.1 we linearize the field equations and set up the perturbative analysis, which is carried out in Section 3.2 for tensor and vector perturbations. No instabilities are found in these sectors. The lowest tensor modes arise from metric perturbations, while the lowest vector modes are the expected massless Kaluza-Klein vectors for the internal S 7 , which here arise from mixings of metric and form contributions. In Section 3.3 we analyze scalar perturbations. Here we confirm the results in [24]: there are no instabilities in the = 0 sector, where the available modes arise from the metric tensor and the dilaton, while there are instabilities for = 2, 3, 4, where also the form field comes into play. However, we display a wide corner of modified potentials, which lie close to the lowest-order one in eq. (1.1) but have a negative V 0 , where no unstable modes are present. At the end of the section we point out how the instabilities could be removed via projections in the internal sphere for the original potential (1.1), although all examples that we have constructed feature fixed sub-varieties. In Section 4 we review the AdS 7 × S 3 heterotic vacua of [11] and extend them in the most general way that is of interest with constant dilaton profiles, allowing again for generic values of the potential V 0 , its first derivative V 0 and its second derivative V 0 . In Section 4.1 we linearize the field equations and set up the perturbative analysis, which is carried out in Section 4.2 for tensor and vector perturbations. Again, no instabilities are found in these sectors. The lowest tensor and vector modes are massless spin-two excitations and the expected massless Kaluza-Klein vectors for the internal S 7 , which here arise, again, from mixed metric and form contributions. In Section 4.3 we analyze scalar perturbations and show that there are no instabilities in the = 0 sector, where only the metric tensor and the dilaton enter, while there is again an instability when the form field comes into play. Here it only affects the = 1 modes, and could be removed by an antipodal Z 2 orbifold projection in the internal manifold, along with all odd-harmonics. As for the orientifold vacua, we display however a wide corner of modified potentials that lie close to the lowest-order one in eq. (1.1) and have a negative V 0 , where again no unstable modes are present. In Section 5 we review the vacua with nine-dimensional Poincaré symmetry of [12], and in Section 5.1 we set up the perturbative analysis. Then in Section 5.2 we show that there are no perturbative instabilities in the scalar sector for the potentials in eqs. (1.1) and (1.2), and in Section 5.3 we show that the same is true for vector and tensor perturbations. This background is therefore a perturbatively stable solution of Einstein's equations, although from the vantage point of String Theory it includes strong-coupling regions. In Section 6 we analyze the stability of the linear-dilaton vacua that originate, below the critical dimension of String Theory, from [13,25]. In Section 7 we review the salient features of the climbing scalar cosmologies that arise with the potentials of eqs. (1.1) and (1.2), and in Sections 7.1 and 7.2 we analyze the corresponding perturbations. We show that there is a logarithmic instability for the homogeneous k = 0 tensor mode, but there are none for other modes. In Section 8 we consider the behavior of a class of milder exponential potentials, which can arise in lower dimensions, in the presence of branes, and we show that there are no instabilities for them. Finally, in Section 9 we analyze a special class of potentials related to the linear-dilaton cosmologies of [14], while Section 10 contains a short summary of our results and some indications on possible further developments. There are also four Appendices. In Appendix A we discuss some differential equations that are encountered in Sections 3.3 and 4.3, while in Appendix B we review some properties of tensor spherical harmonics that are used extensively in Sections 3.1 and 4.1. In Appendix C we collect some useful results on BF bounds, along with a sketchy derivation of them, and finally in Appendix D we collect some observations on cosmic and conformal time that are relevant for Section 8.

The Models
In this paper we explore the low-energy dynamics of the three ten-dimensional string models with broken Supersymmetry and no tachyons in their spectra. The first two models are the U Sp(32) orientifold with BSB of [5] and the U (32) orientifold of [7], whose low-energy effective field theories are identical, insofar as the vacua addressed here are concerned, while the third is the SO(16) × SO(16) heterotic model of [9]. In all cases we shall account for their exponential dilaton potentials, whose origin is however different in the orientifold and heterotic examples. In the former it reflects residual brane/orientifold tensions, and is thus an open-string (projective)disklevel effect, while in the latter it arises from the torus and is therefore a standard first quantum correction. As we have shown in [11], these potentials allow AdS 3 × S 7 flux vacua in the two orientifold models and AdS 7 × S 3 flux vacua in the heterotic model. In both classes of vacua the dilaton acquires constant values, which can be tuned into regions of small string coupling.
We use the "mostly plus" signature and the following definition of the Riemann curvature in terms of the Christoffel connection (M, N = 0, ..9): is the Ricci tensor. Notice that with this definition the curvature of a sphere is negative, and that the relation to R M N AB (ω), the curvature in the frame formalism, is Here we refer to the curvature defined in terms of Γ, and in our conventions The low-energy dynamics of the systems of interest is captured by a class of Lagrangians involving the metric tensor, a scalar field φ and a two-form gauge field of field strength H 3 . In the Einstein frame, these read The equations of motion read, in general, Equivalently, one can combine the Lagrangian Einstein equation with its trace and work with The orientifold AdS 3 ×S 7 vacua of interest are supported by a flux of the three-form field strength H µνρ in the AdS factor, while their heterotic counterparts are supported by a flux of the threeform field strength H ijk in the S 3 factor.
Actually, it proved very instructive to allow generic values, in the vacuum, of the potential V 0 and of its first and second derivatives V 0 and V 0 . As we shall see, while instabilities are present, among the available scalar perturbations, in the uncorrected vacua corresponding to eqs. (2.6) and (2.7), nearby interesting regions of stability exist with V 0 < 0. We also extended the discussion to more general systems, allowing generic values of β, but this did not add significant novelties to the picture.
The ensuing sections are devoted to the study of perturbations of the two classes of AdS × S backgrounds described in the Introduction. In the following, we shall thus refer all covariant derivatives to the corresponding background metrics. Moreover, we shall distinguish space-time d'Alembertians, denoted as usual by 2, and internal Laplace operators, here denoted by ∇ 2 , since we shall decompose all perturbations in the proper sets of internal spherical harmonics, on which ∇ 2 has the eigenvalues discussed in Appendix B.

The (Generalized) AdS × S 7 Orientifold Flux Vacua
The background manifold is in this case AdS 3 × S 7 , with metric Here λ and γ are AdS 3 and S 7 metrics of unit radius, while R AdS and R denote the actual AdS 3 and S 7 radii. Greek indices run from 0 to 2, while Latin indices run from 1 to 7, the dilaton has a constant vacuum value φ 0 , and finally there is three-form flux in AdS, with Here h is a constant and 012 = 1 = − 012 , while all other components of H M N P vanish in the vacuum.
For maximally symmetric spaces, in terms of R(Γ), where R and R AdS are the radii of the sphere and AdS factors. Moreover, the preceding conventions imply that where, here and in the following Section 3.3, covariant derivatives are computed referring the AdS 3 × S 7 background. In addition, the zeroth-order dilaton equation gives which links the three-form flux, sized by h, to the derivative of the scalar potential. Notice that the allowed signs of V 0 and β must coincide, a condition that holds for the perturbative orientifold vacuum, where β = 1. The Einstein equations translate into 15 and it is convenient to define the two variables which will often appear in the next section. Notice that σ 3 ≥ 1 and 9) so that the value σ 3 = 4 3 separates negative and positive values of V 0 for these generalized AdS 3 ×S 7 vacua, and for the (projective)disk-level orientifold potential (3.10)

Perturbations of the Generalized AdS 3 × S 7 Orientifold Flux Vacua
We can now discuss perturbations in these vacua, letting 11) and linearizing the resulting equations of motion. The perturbed tensor equations are where, here and in the following, 13) in terms of the AdS and sphere contributions. In a similar fashion, the perturbed dilaton equation Finally, the perturbed metric equations that follow from eq. (2.9) rest on the linearized Ricci and read In all cases, perturbations depend on the AdS coordinates x µ and on the sphere coordinates y i , and will be expanded in corresponding spherical harmonics, whose structure is briefly reviewed in Appendix B. For instance, for internal scalars this will always result in expressions of the type 8) (y) , (3.17) where I i = 1, . . . , 8 and h µν, I 1 ...I (x) is totally symmetric and traceless in the Euclidean I i labels.
However, the eigenvalues of the internal Laplace operator ∇ 2 will only depend on . Hence, for the sake of brevity, and at the cost of being somewhat sketchy, we shall leave the internal labels implicit, although in some cases we shall refer to their ranges when counting multiplicities.
For tensors in internal space there are some additional complications. For example, for mixed metric components the expansion reads (3.18) where h µJ, I 1 ...I (x) corresponds to a "hooked" Young tableau of mixed symmetry and ≥ 1, as explained in Appendix B. Here the Y (8) i are vector spherical harmonics, and we shall drop all internal labels, for brevity, also for the internal tensors that we shall consider.

Tensor and Vector Perturbations
Following standard practice, we classify perturbations referring to their behavior under the isometry group SO(2, 2) × SO(8) of the AdS 3 × S 7 background. In this fashion, the possible unstable modes violate the BF bounds, which depend on the nature of the fields involved and correspond, in general, to finite negative values for (properly defined) squared AdS masses. Indeed, as reviewed in Appendix C with reference to forms, care must be exercised to identify the proper masses to which the bound applies, since in general they differ from the eigenvalues of the corresponding AdS d'Alembertian. In particular, aside from the case of scalars, massless field equations always exhibit gauge symmetries.
Let us begin by considering tensor perturbations, which result from transverse traceless h µν , with all other perturbations vanishing. The corresponding dynamical equation where we have replaced the internal radius R with the AdS radius R AdS using eq. (3.8), obtains when the first of (3.16) is combined with the results summarized in Appendix B on general spherical harmonics. These harmonics are eigenvectors of the internal Laplace operator in eq. (3.13), whose eigenvalues on SO(8) scalars are − ( +6) R 2 , with = 0, 1, ... an integer number. In order to properly interpret this result, however, it is crucial to notice that the massless tensor equation in AdS is the one determined by gauge symmetry. In fact, the linearized Ricci tensor determined by eq. (3.15) is not gauge invariant under linearized diffeomorphisms of the AdS background, but (3.20) However, the fluxes present in eq. (2.9) endow, consistently, its r.h.s. with a similar behavior, and = 0 in eq. (3.19) corresponds precisely to massless modes. Thus, as expected from Kaluza-Klein theory, eq. (3.19) describes a massless field for = 0, and an infinity of massive ones for > 0. These perturbations are all consistent with the BF bound, and therefore no instabilities are present in this sector.
There are also scalar excitations resulting from the traceless part of h ij that is also divergencefree, which are tensors with respect to the internal rotation group. They satisfy (see Appendix B) 21) so that their squared masses are all positive. Finally, there are massive b ij perturbations, which are divergence-free and satisfy Vector perturbations are a bit more involved, due to mixings between h µi and b µi induced by fluxes. The relevant equations are where h µi and b µi are divergence-free in both indices. It is now possible to write but this does not determine F β i uniquely, since the redefinitions do not affect b µi . The divergence-free b µi of interest obtain, in particular, provided F β i is divergence-free in its internal index i, and divergence-free Λ i do not affect this condition.
One is thus led to the system 2 3.26) and the first of eqs. (3.26) could in principle accommodate a source term of the type ∇ µ Λ i .
However, its contribution can be absorbed by a gauge redefinition of the type (3.25), and from now on we shall ignore it. Similar arguments apply to the ensuing analysis of scalar perturbations in this section and to some cases in Section 4.
In terms of the combination σ 3 of eq. (3.8) this system becomes The eigenvalues of the mass matrix are thus In order to refer to the BF bound in Appendix C, one should add 2 to these expressions and compare the result with zero. All in all, there are no modes below the BF bound in this sector.
The vector modes lie above it for > 1 in the region σ 3 > 1, while they are massless for = 1 and all allowed values of σ 3 > 1, and also, for all , in the singular limit σ 3 = 1, which would translate into a seven-sphere of infinite radius. For = 1 there are 28 massless vectors arising from one of the eigenvalues above. Indeed, according to Appendix B they build up a secondrank antisymmetric tensor in internal vector indices, and therefore an adjoint multiplet of SO (8) vectors. This counting is consistent with Kaluza-Klein theory and reflects the internal symmetry of S 7 , although the massless vectors originate here from mixed contributions of the metric and the two-form field.

Scalar Perturbations
Let us now focus on scalar perturbations of the complete system. To begin with, b µν contributes to scalar perturbations, as can be seen letting 29) an expression that satisfies identically On the other hand, they do not arise from b µi and b ij , since the corresponding contributions would be pure gauge. On the other hand, scalar metric perturbations can be parametrized as up to a gauge transformation with independent parameters along AdS 3 and S 7 directions. The linearized b µν tensor equation yields where we use the decomposition of eq. (3.13), so that ∇ 2 denotes the internal background Laplacian. After expanding in internal spherical harmonics, so that ∇ 2 → − ( +6) R 2 , eq. (3.32) becomes finally (an AdS derivative of) Notice that a redefinition B → B + f (y), where f (y) depends only on internal coordinates, would not affect b µν in eq. (3.29). As a result, while eqs. (3.32) and (3.33) could in principle contain a source term, this can be eliminated taking this fact into account. Similar considerations will apply for the B field in Section 4.3.
In a similar fashion, the dilaton equation becomes 34) or, after combining it with eq. (3.33), Finally, after eliminating 2 B with eq. (3.33), the metric equations (3.16) read These equations have an unfamiliar form, and for this reason in Appendix A we prove that the terms involving gradients must vanish separately. One ought nonetheless to distinguish two cases.
For = 0 nothing depends on internal coordinates, the terms involving ∇ µ ∇ i and ∇ i ∇ j become empty and D also disappears. According to Appendix A, in this case one is thus led to the reduced 37) to be supplemented by the linear relation Using the definitions of σ 3 and τ 3 , eqs. (3.37) can be recast in the form 39) and the last column of the resulting mass matrix vanishes, so that there is a vanishing eigenvalue whose eigenvector is proportional to B. This perturbation is however pure gauge, since eq. (3.29) implies that the corresponding field strength vanishes identically. Leaving it aside, one can work with the reduced mass matrix (in our (2−M 2 ) convention) determined by the other two equations, whose eigenvalues are There are regions of instability as one varies the parameters, but for the actual orientifold potential, where (β, σ 3 , τ 3 ) = 1, 3 2 , 9 2 , the two eigenvalues, are positive, and thus lie well above the Breitenlohner-Freedman bound. To reiterate, there are no unstable scalar modes for the BSB flux vacuum in the = 0 sector for the internal S 7 . In view of the ensuing discussion, let us add that the stability persists for convex potentials, with τ 3 > 0, independently of σ 3 .
For = 0 the system becomes more complicated, since it now includes the two algebraic constraints A + 7 C + 2 ( + 6) D = 0 , 43) and the five dynamical equations

AdS
, and the BF bound is -1 in this case. Notice the peculiar behavior, already spotted in [24], whereby the squared masses decrease initially, rather than increasing, as increases between 1 and 3.
Let us first notice that this set of seven equations for the five unknowns (A, B, C, D, ϕ) is consistent: one can indeed verify that eqs. (3.44) respect identically the algebraic constraints of eqs. (3.43). One can thus concentrate on the three equations for (A, ϕ, B), which do not involve other fields and read where we have introduced the shorthand notation to then determine C and D via the algebraic constraints. AdS M 2 and the BF bound, which is -1 in this case. There are regions of stability for values of σ 3 close to 1, which correspond to R 2 R 2 AdS > 9 and negative values of V 0 . The example displayed here refers to = 3, which corresponds to the minimum in the orientifold case of fig. 1, and the peak identifies the point corresponding to the tree-level values σ 3 = 3 2 , The mass matrix of interest is therefore where now L 3 = 0. In all cases one is to compare the squared mass eigenvalues with the Breitenlohner-Freedman (BF) bound for scalar perturbations, which in this AdS 3 × S 7 case reads ( 3.48) For the BSB case, one is thus led, in agreement with [24], to the simple results (3.49) and the BF bound is thus violated by the third eigenvalue for = 2, 3, 4. Decreasing the value of β could remove the problem for = 4, but the instability would still be present for = 2, 3. On the other hand, increasing the value of β instabilities show up also for higher values of .

Figure 3: A different view. Comparison between the lowest eigenvalue of R 2
AdS M 2 and the BF bound, which is -1 in this case, as a function of and σ 3 , for τ 3 = 9 2 . There are regions of stability for values of σ 3 close to 1, which correspond to large values for the ratio R 2 R 2 AdS and to negative values of V 0 .
The issue of interest is now whether there exist regions within the parameter space spanned by σ 3 and τ 3 where the violation does not occur. We did find them, for all dangerous values of , for values of σ 3 that are close to one, and therefore for negative V 0 , and for positive τ 3 , i.e.
for potentials that are convex close to the vacuum configuration. These results are displayed in figs. 2 and 3.
One can try to eliminate the unstable modes present for = 2, 3, 4 by projections in the internal S 7 , which can be embedded in C 4 constraining its four complex coordinates Z i to satisfy (3.50) According to Appendix B, scalar spherical harmonics of order are harmonic polynomials of degree in the Z i and their complex conjugates, so that the issue is how to project out the dangerous ones. The three-sphere, which can be embedded in C 2 demanding that provides an instructive simpler case. One can indeed associate each point on S 3 to a quaternion of unit norm on which the SU (2) rotations act freely. One can verify that these rotations, when composed in all possible ways, build the symmetry group of the cube in the three-dimensional Euclidean space associated to the three generators σ i 2 . One can also show that these operations suffice to eliminate all harmonic polynomials of degrees ≤ 4, while leaving no fixed sub-varieties on account of their free action on quaternions by left multiplication. One would naturally expect octonions of unit norm to play a similar role for S 7 , but have just taken a cursory look at this construction. Alternatively, and more simply, one could consider the transformations generated by the R i in eq. (3.53) acting simultaneously on complementary pairs of (Z i , Z j ) coordinates. This would suffice to eliminate all unwanted spherical harmonics, but unfortunately it would also generate fixed sub-varieties.
At any rate, one should eventually exclude non-perturbative instabilities of the type discussed in [30], and we leave to future work the analysis of all these issues. String corrections, which could drive the potential to a nearby stability domain, provide in our opinion an interesting alternative for these AdS 3 × S 7 orientifold vacua.

The (Generalized) AdS 7 × S 3 Heterotic Vacua
In these vacua there are a few novelties with respect to the orientifold case, since, which will have nonetheless some relevant effects. In the notation of Section 2, now β = −1, while With this proviso, the equations of motion are again (2.8) and (2.9), but in this case the flux is in the internal sphere. Therefore eq. (2.8) becomes which is solved by Consequently, the scalar equation gives again while the Einstein equations translate into Notice that this solution demands that β V 0 < 0, and for later convenience we also define For these vacua σ 7 ≥ 3, while the sign of τ 7 is a priori arbitrary. Moreover, 8) which changes sign at σ 7 = 12, and finally for the torus-level heterotic potential

Perturbations of the Generalized AdS 7 × S 3 Heterotic Flux Vacua
In this case the perturbed tensor equations take the form while the perturbed dilaton equation is now Finally, the perturbed metric equations that follow from eq. (2.9) rest on eq. (3.15) and read In all cases, perturbations depend on the AdS coordinates x µ and on the sphere coordinates y i , and will be expanded in the corresponding spherical harmonics, whose structure is briefly reviewed in Appendix B, proceeding as in Section 3.1.

Tensor and Vector Perturbations
To begin with, let us notice that tensor perturbations, which result from transverse traceless h µν when all other perturbations vanish, satisfy in these AdS 7 vacua the equation For = 0, this describes a massless graviton field, which is accompanied by a tower of Kaluza-Klein states for higher . Hence, there are no instabilities in this sector.
There are massive scalar excitations resulting from the traceless part of h ij that is also divergence free, which is a tensor with respect to the internal rotation group. They satisfy so that the results in Appendix B imply that no instabilities are present also in this sector. There are also no unstable modes from transverse b µν excitations, which satisfy, 15) so that the lowest ones, corresponding to = 0, are massless.
Vector perturbations are more involved, since there are mixings between h iµ and b iµ . In order to study them, one can proceed in analogy with Section 3.2, letting 3 (4.16) which is transverse in internal space. The resulting system reads 17) and the eigenvalues are

Scalar Perturbations
Proceeding as in the preceding sections, let us now concentrate on scalar perturbations starting from One can describe scalar perturbations letting 20) a choice that also satisfies In addition, let us parametrize scalar metric perturbations as 22) along the lines of what we did in the preceding sections.
In this fashion, the first of eqs. (4.10) turns into which is now present only for l = 0, while the complete scalar equation reads For scalar perturbations one can thus obtain where we have eliminated 2 D from the tensor equation. Although there are seven equations for five unknowns, one can verify that the system is consistent. All in all, one can thus work with (C, ϕ, B), restricting the attention to which are here expressed in terms of the two variables σ 7 and τ 7 of Section 4, to then determine A and D algebraically, and where for brevity we have let To begin with, let us notice that for = 0 B decouples, so that the system reduces to In terms of the σ 7 and τ 7 variables of Section 4, the mass matrix thus reads AdS M 2 and the BF bound, which is -9 in this case. There are regions of stability for values of σ 7 close to 3, which correspond to R 2 R 2 AdS > 9, and to negative values of V 0 . The example displayed here refers to β = −1 and = 1, which corresponds to the minimum in the heterotic case of fig. 4, and the peak identifies the point corresponding to the tree-level values σ 7 = 15, τ 7 = 75. 29) and its eigenvalues are They are both positive for the tree-level effective Lagrangian, and for the heterotic potential, for which they read We can now move on to the = 0 case, where the three functions (C, φ, B) all contribute, so that one is led to the mass matrix (4.33) Figure 6: A different view. Comparison between the lowest eigenvalue of R 2 AdS M 2 and the BF bound, which is -9 in this case, as a function of and σ 7 , for τ 7 = 75. There are regions of stability for values of σ 3 below 12, which correspond to relatively large values for the ratio R 2 Still, there is again a stability region for values of σ 7 that are close to 12, for negative V 0 , and typically for positive τ 7 , i.e. for potentials that are convex close to the vacuum configuration..
These results are displayed in figs. 5 and 6.
In this case one could eliminate the bad eigenvalue by a Z 2 antipodal projection in the internal sphere S 3 , which can be identified with the SU (2) group manifold. This operation has no fixed points, and reduces the internal space to the SO(3) group manifold, without affecting the massless vectors with = 1 that we have identified. Alternatively, one could resort to the symmetry group of the sphere related to the action on unit quaternions that we have described for the orientifold vacua. The resulting settings, however, resonate again with the discussion in [30], and nonperturbative instabilities are in principle relevant to the story, so that we leave an analysis of this problem to future work. String corrections would also deserve a closer look, since they could drive the potential to a nearby stability domain, providing an interesting alternative for these AdS 7 ×S 3 heterotic vacua.

The 9D Dudas-Mourad Non-Supersymmetric Vacua
Our starting point is now provided by the classical solutions of [12] for the ten-dimensional Sugimoto orientifold [4], which in the Einstein frame read where the absolute values would not be needed here, since y ∈ (0, ∞), but this notation will be convenient in the following section. The corresponding Einstein-frame expressions for the These two vacua have nine-dimensional Poincaré symmetry, while their internal spaces are actually intervals of finite length in the metrics of eqs. (5.1) and (5.2). It is convenient to recast the two solutions in terms of conformally flat metrics, so that one is led to consider expressions of the type In detail, in the orientifold case the coordinate z is obtained integrating the relation On the other hand, in the heterotic case and Notice that one is confronted with an interval whose finite length is proportional to in the two cases, but which hosts a pair of metric singularities at its two ends y = 0 and y = +∞, with a string coupling that is weak at the former and strong at the latter. Moreover, the parameters α O and α H are proportional to the residual tension, and therefore the supersymmetric case corresponds to the singular limit as they tend to zero, where the internal length diverges.

Perturbations of the 9D Vacua
The equations of interest are now 8) and the corresponding perturbed fields take the form As a result, the perturbed Ricci curvature can be extracted from an expression where covariant derivatives do not involve Ω, and thus refer to η M N + h M N , which is also used to raise and lower indices. Up to first order the metric equations of motion thus read 11) and combining this result and the scalar equation in (5.8) yields the unperturbed equations of 9 where V and V φ denote the potential and its derivative computed on the classical vacuum. Notice that the first two equations can be equivalently recast in the form 16) and that the equation for φ is a consequence of these.
All in all, (5.11) finally leads to

Scalar Perturbations
For scalar perturbations 20) with p µ p ν η µν = −m 2 and p.x = p µ x ν η µν , so that the Einstein equations become while the perturbed scalar equation reads Substituting the preceding expressions and using the background equations now gives 25) and altogether the four scalars A, C, D and φ obey the linearized equations Notice that some of the metric equations, the second one and the third one above, are constraints, and that there is actually another constraint that obtains combining the first and the last so as to remove A . Moreover, eq. (5.25) is a consequence of these.
The system, however, has a residual local gauge symmetry, a diffeomorphism of the type z = z + (x µ , z) , (5.27) which is available in the presence of a single internal dimension and implies Taking into account the original form of the metric in eq. (5.9), which in terms of our perturbations reads ds 2 = e 2Ω(z) (1 + A) dx µ dx µ + 2 dx µ dz ∂ µ D + (1 + C) dz 2 , (5.29) one can thus identify the transformations Notice that D behaves as a Stückelberg field, and can be gauged away, leaving only one scalar degree of freedom after taking into account the constraints, as expected from Kaluza-Klein theory.
After gauging away D the second of eqs. (5.26) implies that while the third of eqs. (5.26) implies that There is nothing else, since differentiating the third of eqs. (5.26) and using the background equations gives Taking this result into account, one can verify that the last of eqs. (5.26) also leads to (5.33), whose properties we now turn to discuss.
The issue at stake is again the stability of the solution, which in this case reflects itself in the sign of m 2 : a negative value would signal a tachyonic instability in the nine-dimensional Minkowski space. Changing parameters in the potential is more complicated in this case, since the background values depend on z, but nonetheless we can show that the solution corresponding the lowest-order level potentials is stable, in both the orientifold and heterotic models. To this end, let us recall that a generic second-order equation of the type One is thus led to and tracing the preceding steps one can see that Ψ is in L 2 . Eq. (5.37) can be conveniently discussed connecting it to a more familiar problem of the type where Once these relations are supplemented with Neumann or Dirichlet conditions at each end in z, one can conclude that in all these cases which is again non negative, so that the heterotic vacuum is also a perturbatively stable solution of the Einstein-dilaton system for all allowed choices of boundary conditions at the ends of the interval. The presence of regions where world-sheet or string loop corrections are large, however, makes the lessons of these results less evident for String Theory.

Tensor and Vector Perturbations
Tensor perturbations are simpler to study, and to this end one only allows a transverse traceless h µν . After a Fourier transform one is thus led to with Dirichlet or Neumann boundary conditions the argument of Section 5.2 applies, and one gets a discrete spectrum of masses. Moreover, one can verify that there is a normalizable zero mode with h µν independent of z, which signals that at low energies gravity is effectively nine dimensional.
As in previous cases, vector perturbations entail some mixings, because in this case they originate from transverse h µ9 and from the traceless combination (5.48) so that The relevant vector is (5.50) which satisfies the two equations the first of which is clearly solved by with a constant C µ . In analogy with the preceding discussion, one might be tempted to identify a massless vector. However, one can verify that, contrary to the case of tensors, this is not associated to a normalizable zero mode. The result is consistent with standard expectations from Kaluza-Klein theory, since the internal manifold has no translational isometry.

The Linear-Dilaton Vacua
Variants of this setting encompass the case of non-critical strings, lower-dimensional compactifications of the ten-dimensional models that we are analyzing in the presence of an internal breathing mode, and also the very important case of cosmological perturbations in four dimensions. In particular, one can describe non-critical strings starting from (6.2) with α > 0 for d > 10 and α < 0 for d < 10. Moreover for the potentials arising from the Polyakov measure [25].
The equations of motion read (6.4) and the corresponding perturbed fields take again the form 6.5) while the perturbed Ricci curvature can be extracted from The unperturbed equations of motion then read 7) where, as in the preceding section, V and V φ denote the potential and its derivatives, computed on the classical vacuum. The background solution that we are after in this section is the lineardilaton vacuum discussed in [13], which is an exact classical solution of String Theory, to all orders in α . The corresponding field profiles are (6.8) where the parameter a is determined by the potential in eq. (6.1) according to (6.9) Proceeding as in the preceding section, one is thus led to the equation of scalar perturbations (6.10) where the relations between C, A and ϕ are now In a similar fashion, tensor perturbations are described by (6.12) For the linear dilaton solution of eqs. (6.8) and (6.9), eqs. (6.10) and (6.12) become identical and take the simple form (6.13) Retracing the preceding steps one is thus led to define (6.14) and then (6.15) which admits bounded solutions only if Therefore, this linear-dilaton background is stable. However, it has several problems. To begin with, although eqs. (6.8) and (6.9) correspond to an exact solution of tree-level String Theory to all orders in α , there is a region of strong coupling for large negative values of z, and moreover the preceding argument shows that there are no massless scalar or tensor modes around this vacuum.
In addition, from a lower-dimensional perspective there is a continuum of massive excitations.

The Dudas-Mourad Cosmological Solutions in Ten Dimensions
Our starting point is now the analytic continuation under y → it, and consequently under z → iη, of the classical solutions of Section 5. For the ten-dimensional Sugimoto orientifold [4] one thus obtains, in the Einstein frame, Both cosmologies have a nine-dimensional Euclidean symmetry, and in both cases, as shown in [16], the dilaton is forced to emerge from the initial singularity climbing up the potential. In this fashion it reaches an upper bound, which translates into an upper limit on the string coupling, before it begins its descent.
It is convenient to recast these expressions in conformal time according to In the orientifold case the conformal time η is obtained integrating the relation (7.4) and (7.5) while in the heterotic case (7.6) and In both models one can choose the range of η to be (0, ∞), with the initial singularity at the origin. Moreover, as we have stressed, in both cases the dilaton, and thus the string coupling, is bounded from above, so that string loops are in principle under control. However, there is still a singularity at t = 0 where string world-sheet corrections, which are not taken into account in this Supergravity approximation, are expected to play an important role [20].

Tensor Perturbations
The issue at stake, here and in the following sections, is whether or not solutions determined by arbitrary initial conditions provided some time after the initial singularity can grow in the future evolution of the Universe. This can be done relatively simply at large times, which translate into large values of the conformal time η, where many expressions simplify. Moreover, for finite values of η the geometry is regular and the coefficients in eq. (7.8) are bounded, so that the solutions are also not singular. However, an O(1) growth is relevant for perturbations, and therefore we shall begin with the asymptotics and then, at the end of the section, we shall also take a global look at the problem.
In the ten-dimensional orientifold and heterotic models of interest, using spatial Fourier transforms and proceeding as in the preceding section, one can show that tensor perturbations evolve according to (7.8) where "primes" denote derivatives with respect to the conformal time η. Let us begin by noting that, for all exponential potentials 7.9) with γ E ≥ 3 2 , and therefore for the orientifold potentials of [5] and [7], which have γ E = 3 2 and are "critical" in the sense of [16], but also for the SO(16) × SO(16) heterotic string of [9], which has γ E = 5 2 and is "super-critical" in the sense of [16], the solutions of the background equations (7.11) In the picture of [16], in this region the scalar field has overcome the turning point and is descending the potential, so that the supergravity approximation is expected to be reliable, but the potential contribution is manifestly negligible only for the "super-critical" heterotic potential (1.2), where e 2Ω V decays faster than 1 η 2 for large η. However, the result also applies for γ E = 3 2 , which marks the onset of the "climbing behavior". This can be appreciated retaining subleading terms, which results into (7.12) so that the potential decays as 13) which is faster than 1 η 2 .
Notice that a similar behavior, but with the scalar climbing up the potential, (7.14) also emerges for small values of η, for all γ E ≥ 3 2 , and thus in all orientifold and heterotic models of interest. However, these expressions are less compelling, since they concern the onset of the climbing phase. The potential is manifestly subdominant for small values of η, but curvature corrections, which would be important in this region, are not simply taken into account.
In conclusion, for γ E ≥ 3 2 and for large values of η eq. (7.11) holds and eq. (7.8), which describes tensor perturbations, therefore approaches Consequently, for k = 0 (7.16) and the oscillations are damped for large times, so that no instabilities arise. On the other hand, an intriguing behavior emerges for k = 0, which is worthy of some attention in our opinion. In this case the solution of eq. (7.15) implies that 17) and therefore spatially homogeneous tensor perturbations experience in general a logarithmic growth.
This result indicates that homogeneity is preserved while isotropy is generally violated in the tendimensional "climbing-scalar" cosmologies [16] that emerge, in String Theory, in the presence of supersymmetry breaking.
One can actually get a global picture of the phenomenon: eq. (7.15) can be simply solved in terms of the parametric times of [12] for k = 0, and for the U Sp (32) and U (32) orientifold models, while (in this case 0 for the SO (16)  variations toward the end of the climbing phase, where curvature corrections to Supergravity do not dominate the scene anymore, providing some additional support to the present analysis. We are therefore inclined to speculate that the violation of isotropy that we are exhibiting could have left behind some space-time dimensions at a very Early Epoch, opening the way to an effective four-dimensional Universe. 4 While perturbation theory is at most a clue to this effect, the resulting picture is clearly enticing, and moreover, as we shall see shortly, the dynamics becomes potentially richer and stable in lower dimensions, where other branes that become space filling can inject an inflationary phase devoid of this type of instability.
These amusing properties apply to all "(super)critical" exponential potentials 5 7.20) with γ E ≥ 3 2 , where the climbing phenomenon occurs. In all these cases, the potential energy becomes subdominant in the large-η descending phases, so that some aspects of these systems are captured by fluids with an equation of state p = γ ρ , (7.21) with a parameter γ that approaches one from below. This limiting behavior emerges whenever a positive potential becomes subdominant, since in general for a scalar field (7.22) with T and V the corresponding kinetic and potential energies. It is thus instructive to take a cursory look at corresponding Freedman-Robertson-Walker cosmologies in d dimensions, for which (7.23) so that in conformal time Tensor perturbations would evolve in this background according to eq. (8.5), a slight modification of eq. (7.8), as we shall see in Section 8, and the result for homogeneous perturbations would be (7.25) Therefore, in the standard region γ < 1 one would always end up with bounded perturbations at large times, even for k = 0. On the other hand, the behavior in eq. (7.17) would always present itself for γ = 1, while negative potentials would give rise to γ > 1, and thus to worse instabilities.
To reiterate, the instability in the homogeneous tensor modes that we have exhibited for climbing scalars with γ E ≥ 3 2 signals a problem with isotropy that is common to all ten-dimensional string models with broken supersymmetry. As we have already stressed, this points naturally to an awaited tendency toward lower-dimensional space times, albeit without a selection criterion for the resulting dimension d < 10. Hence, if the picture that we are advocating were correct, the selection of a four-dimensional Universe in String Theory would be an accident, no more and no less than in other contexts, but with hints from the breaking of Supersymmetry that point to its inevitable emergence. Before proceeding to examine lower-dimensional settings, let us take a look at scalar perturbations in ten dimensions.

Scalar Perturbations
Scalar perturbations exhibit a very different behavior in the presence of the exponential potentials (7.20) with γ E ≥ 3 2 , and in particular of those in eqs. (1.1) and (1.2) that reflect the breaking of Supersymmetry in ten-dimensional String Theory. Our starting point is the analytic continuation of eq. (5.33) under z → i η, which reads (7.26) As in eq. (7.8), m 2 was also replaced with −k 2 , which originates from a spatial Fourier transform, and "primes" denote again derivatives with respect to the conformal time η.
As we have stressed in the preceding section, the potential is subdominant in eq. (7.26) for γ E ≥ 3 2 , which leads to the asymptotic behaviors of eqs. (7.14) during the climbing phase, and of eqs. (7.11) during the descending phase. As a result, during the latter eq. (7.26) reduces to (7.27) whose solution is For k = 0 the amplitude always decays proportionally to (η) − 3 2 , while for k = 0 the two independent solutions of eq. (7.26) are dominated by Therefore, scalar perturbations do not grow in time, even for the homogeneous mode with k = 0, for γ E ≥ 3 2 , and thus, in particular, for the U Sp (32) and U (32) orientifold models of [5] and [7], and also for the SO(16) × SO(16) heterotic model of [9].

A Family of Cosmologies in d Dimensions
In Section 7.1 we have noticed that homogeneous tensor perturbations develop an instability in the ten-dimensional potentials of eqs. (1.1) and (1.2), and we have emphasized that this breakdown of isotropy could have ignited the transition to a four-dimensional Universe. Here we would like to explore cosmological perturbations in the richer dynamical settings that become available for d < 10. The picture that we have in mind is that these more general potentials could have driven the scalar field along them during its descent, and in this spirit we shall explore whether instabilities arise in this dynamical regime.
We have actually in mind two types of action principles. The first is the naive extension to d < 10 of eq. (2.5), considered however for a "mild" (in a sense to be specified shortly) positive exponential potential characterized by a parameter γ. In contrast, the ten-dimensional models contained two types of "hard" potentials, which we first met in eqs. (1.1) or (1.2). We shall leave these contributions implicit here: their main lesson, the inevitable presence of an early climbing phase, was already taken into account. The second type of action, captures lower-dimensional mixings between the dilaton and the breathing mode of the internal manifold [17]. This second option is relevant after the compactification, up to another orthogonal mixing of dilaton and breathing mode that, as in [17], we shall assume to be somehow stabilized and foreign to the dynamics. Clearly, we cannot nearly claim full control of all this interesting dynamics, not even within Supergravity, but we shall attempt nonetheless to extract potentially useful indications from it, within this assumption.
Notice also that the two actions of eqs. (8.1) and (8.2) can be simply turned into one another by a redefinition of φ, which also connects γ d to γ according to 6 One can thus explore their indications simultaneously, starting from the background equations, which in these lower-dimensional settings read (8.4) Starting from the results of Section 6, one can also show that the tensor perturbations of the Lagrangian (8.1) satisfy while the corresponding scalar perturbations satisfy As we have anticipated, we shall focus on dynamics that are dominated by a single "mild" exponential term, so that the asymptotic solutions of eqs. (8.4) for large values of η, in the region where the scalar descends the potential, are quite different from what we saw in preceding sections, and These results describe the Lucchin-Matarrese attractor [33] in d dimensions, a special solution that captures the large-time behavior of all solutions of the gravity-scalar system in the presence of "mild" positive exponential potentials 7 This qualification, as we can now see, translates into the condition γ < γ (c) , (8.10) since the solutions in eq. (8.9) exist, for positive potentials, only within this range.
Making use of these results in eqs. (8.5) and (8.6) leads to two very similar equations, where (8.14) Denoting the corresponding fields collectively as Y , the solutions can be presented in the form Exponential potentials in Cosmology have a long history, and some relevant previous work can be found in [34].
for k = 0, and Y (η) = D 1 |η| 1−a + D 2 (8.16) for k = 0, with a = a T for tensor perturbations and a = a S for scalar ones. Notice that for γ > γ the Universe undergoes a decelerated expansion, and therefore we are interested in the behavior as η → ∞, while if γ < γ it undergoes an accelerated expansion, and therefore we are interested in the behavior as η → 0.
Leaving aside momentarily the case γ = γ , to which we shall return in the next section, one can simply verify that perturbations never grow (when d > 2) if eq. (8.10), which is instrumental for the existence of the Lucchin-Matarrese attractor with positive potentials, holds. To reiterate, no instabilities arise, even for homogeneous perturbations, in the presence of a "mild" exponential potential. Notice also that, in the picture subsumed by eq. (8.2), γ (c) becomes the "critical" value of [17].
As in Section 7.1, one can get a simple global view of the homogenous solutions of eq. (8.5).
This is determined by the first integral of eqs. (8.11) and (8.12) dh ij = C ij e −(d−2)Ω dη , (8.17) where C ij is a constant matrix, an equation that can be simply integrated working in terms of the parametric time of [12]. The starting point in this case is provided, in the notation of [16], by but the scalar field and the parametric time were redefined there in such a way that the transition to the "climbing behavior" occurred, for any value of the dimension d, for γ = 1. The translation into the present notation rests on the redefinitions 19) and taking them into account leads, for homogeneous tensor perturbations, to the result (8.20) where α O,H stands for α O in the orientifold case and for α H in the heterotic case. This expression displays clearly that during the descent, the region of interest for the present considerations, this homogeneous perturbation does not grow appreciably, so that no instabilities arise in homogenous tensor perturbations for γ < γ (c) . This is as expected, due to the attractor nature of the Lucchin-Matarrese solution.
What are the relevant values of γ d γ (c) that result from lower-dimensional branes? This was discussed in [17], under the assumptions that were spelled out after eq. (8.2). In our current notation the answer in four dimensions is for a p-brane that couples to the dilaton proportionally to e −σφ . Lower-dimensional non-BPS branes in the string models of interest were discussed in [40], and for instance in four dimensions there is a non-BPS D3 brane of this type, with γ d γ (c) = 1 2 . In general, there is a whole zoo of branes in d < 10, which were studied in detail by Bergshoeff,Riccioni and others [36], so that there are in principle many options for this type of stable dynamics.
Leaving aside the need for further contributions to the potential that are needed to comply with well-known bounds on the tensor-to-scalar ratio r [35], when combining in four dimensions a "hard" exponential with a "mild" term one stumbles on some amusing numerology. The values of γ translate indeed into the spectral index for primordial scalar perturbations, according to 22) and γ d γ (c) = 1 12 would yield n S 0.96. According to eq. (8.21), this result would obtain for α = 2 and p = 4, i.e. for an N S five-brane wrapped around a small defect in the extra dimensions, which would make it effectively look like a four-dimensional extended object. This would be naturally available only for the SO(16) × SO(16) heterotic string of [9], which motivates us to take a closer look at dualities for these non-supersymmetric strings, starting from the original work in [41].

Linear-Dilaton Cosmologies
In the preceding section we left out the special case γ = γ , in which the solutions in eqs. (8.9) become singular. As explained in Appendix D, the solutions in cosmic time are not singular, and the problem arises merely from the definition of conformal time at the transition between accelerated and decelerated cosmologies. The correct procedure to deal with this issue is to look for a different class of solutions of the system (8.4), with φ and Ω constant. These describe the linear-dilaton cosmology of [14] and read where the parameter α is related to the overall strength of the potential in eq. (6.1) according to As a result the equations for scalar and tensor perturbations become identical, and reduce to the simple form 3) whose solutions clearly decay in an expanding Universe for all values of k.
This linear-dilaton background is an exact solution of tree-level String Theory to all orders in α [14], with a strong-coupling region in the infinite past, for large negative values of η, at the initial singularity of the Einstein-frame metric. It is conceivable that string corrections involving higher powers of g s could cure the problem, and the fact that these solutions correspond to string-frame Minkowski metrics appears encouraging to this effect. Once more, the behavior of cosmological solutions of String Theory in the presence of broken supersymmetry appears encouraging.

Conclusions
In this paper we have explored the perturbative stability of four classes of backgrounds that arise when the low-energy effective action of String Theory is supplemented by the dilaton potentials that are by the breaking of Supersymmetry. Our results are as follows.
1. In the AdS 3 × S 7 vacua of the U Sp (32) and U (32) orientifolds of [11] (a) no instabilities are present in AdS tensor and vector modes, and also in the (anti)symmetric tensors in internal space h ij and b ij ; (b) instabilities are present in scalar modes that draw their origin from the dilaton, the metric tensor and the two-form, as explained in Section 3.1. These expand into totally symmetric and traceless SO(8) tensors, and the problem is present for angular momenta corresponding to the three values = 2, 3, 4, in agreement with [24], but have also explored projections of the internal sphere that remove them, perhaps at the price of fixing some sub-varieties. However, even leaving aside the issue of sub-varieties, one ought to investigate vacuum bubbles, which typically occur in Kaluza-Klein theory [29], and vacuum bubbles were indeed shown to destabilize vacua with similar projections in [30]. We leave this problem for future work; (c) wide stability regions exist, however, close to the values of V 0 , V 0 and V 0 for the (projective-)disk potential of eq. (1.1). These regions, where V 0 < 0, could be relevant if corrections are taken into account.
2. The AdS 7 × S 3 vacua of the SO(16) × SO(16) heterotic string display a similar behavior, but: (a) instabilities are present in scalar modes only for = 1, but if the internal sphere is replaced with an orbifold determined by an antipodal Z 2 projection, the unstable modes of the tree-level potential disappear. We leave the problem of vacuum bubbles for future work also in this case; (b) wide stability regions exist again, close to the values of V 0 , V 0 and V 0 for the toruspotential of eq. (1.2). These regions, where V 0 < 0, could again be relevant if corrections are taken into account; 3. the vacua of [12]  5. more general exponential potentials, whose cosmologies were first discussed in [15] and are central to the "climbing scalar" picture of [16], display a sharp change of behavior, in ten dimensions, when the parameter γ E of Section 8 reaches the value 3 2 , where the climbing behavior sets it. Below this "critical" value γ (c) the cosmological solutions approach at large times the d-dimensional counterparts of the Lucchin-Matarrese attractor of [33], and then perturbations do not grow ; 8 6. the special case γ = γ must be treated separately in conformal time, but all perturbations are stable and have a simple behavior. This special value also corresponds to the lineardilaton cosmologies of [14], which arise above the critical dimension of String Theory and are exact tree-level solutions to all orders in α where supersymmetry is broken at the sphere level.
A fair summary of the indications of this work for String Theory is that, while problems emerge in non-supersymmetric flux vacua, the situation appears more natural and promising in evolving cosmological settings. Taking seriously the hint that we gathered in Section 7.1, there would be even clues for the origin of compactification. This all brings to our mind the time-honored case of Newtonian interactions, where static instability can leave way to dynamical stability, with a wealth of manifestations that underlie the Universe up to the largest scales that we have explored to date. Or, for that matter, the case of static Coulomb instabilities, with all they contributed to our understanding of Nature via Quantum Mechanics. Time will tell whether these insights, together with many others that are starting to surface [22], will converge into a main hidden lesson from String Theory.
There are some possible extensions of this work, some of which are under investigation: 1. the general solutions in [11] also included internal gauge fields. These complicate the vacua, and seem not to improve matters for stability, but it may be interesting to complete the analysis; 2. bubble formation can introduce non-perturbative instabilities when internal orbifold projections remove perturbative ones, as in [29]. Taking a closer look at this problem would be particularly relevant for the heterotic AdS 7 ×S 3 vacua, where a simple Z 2 internal projection can remove all unstable modes; 3. in lower dimensions, one could combine Brane Supersymmetry Breaking with Scherk-Schwarz reductions [37], along the lines of what was done for closed strings in [38] and for open strings in [39], and it would be interesting to explore the stability of corresponding vacua; 4. it would be interesting to see how dilaton potentials deform the D p -branes of the models at stake. Without taking these deformations into account, their world-sheet description was presented in [40]; 5. finally, the duality between heterotic and orientifold models becomes perturbative for d < 6, and has already displayed some interesting consequences in the supersymmetric case [43].
The considerations at the end of Section 8, and the apparently richer options allowed for the heterotic SO(16) × SO(16) model, motivate a closer look at the string duality web with broken supersymmetry in d < 10, relying on the steps made in [41].
which appeared recurrently, in the analysis of scalar perturbations, in Sections 3.3,4.3 and 5.2. Referring for definiteness to the first form, we would like to prove that this type of equation implies that A and B must both vanish.
To begin with, one can take a trace, and if the AdS space is of dimension n 1 this gives Next one can take the divergence, obtaining finally Subtracting from this eq. (A.3) one now finds and consequently the original eq. (A.1) can be recast in the form If one now assumes that B = 0, letting C = log B, this result can be turned into Redefining the background metric by a coordinate transformation, one can remove the first term, but the resulting equation is inconsistent, since the l.h.s. is clearly a matrix of lower rank. Hence B = 0 and therefore, a fortiori, A = 0.

Appendix B On Tensor Spherical Harmonics in n Dimensions
In this Appendix we review some results that were needed in our analysis in Sections 3.1 and 4.1, starting from an ambient Euclidean space [26]. The results agree with the constructions presented in [27]. If Y 1 , . . . Y n+1 are Cartesian coordinates of R n+1 , so that the unit sphere S n is described by the quadratic constraint is determined by a totally symmetric and traceless tensor α I 1 ...I of rank , as can be clearly seen applying to it the Laplace operator in Cartesian coordinates.
The scalar spherical harmonics Y I 1 ...I In discussing more general tensor harmonics, it is convenient to notice that, in the coordinate system of eq. (B.7), the non-vanishing Christoffel symbols Γ K IJ for the ambient Euclidean space read Γ r ij = − r g ij , Γ i jr = 1 r δ j i , Γ k ij = Γ k ij . (B.12) The labels i, j, k refer, as above, to the n-sphere, whose Christoffel symbols are denoted by Γ k ij .
The construction extends nicely to tensor spherical harmonics, which can be defined starting from generalized harmonic polynomials, with one proviso. The relation (B.6) and its differentials imply that the actual spherical components of tensors carry additional factors of r, one for each covariant tensor index, with respect to those naively inherited from the Cartesian coordinates of the Euclidean ambient space, as we shall now see in detail. To begin with, vector spherical harmonics obtain starting from one-forms in ambient space, built from harmonic polynomials of the type while the independent perturbations associated to a (p + 1)-form gauge field in the internal space correspond, in general, to multi-row diagrams of the type The degeneracies of these representations can be related to the corresponding Young tableaux, for instance, as in [28]. The structure of the various types of harmonics, which are genuinely different for large enough values of n, reflects nicely the generic absence of mixings between different classes of perturbations.
One can treat the case of a massive vector in a similar fashion, starting from (C.12) To begin with, let us recall that the massive Proca equation implies the divergence-free condition, which in Poincaré coordinates reads (C.13) and that, after letting and for a transverse B the equation of motion can be recast in the form Moreover, in Poincaré coordinates the action takes the form 21) where indices are raised and lowered with a d-dimensional flat metric. Extending the preceding discussion, one can thus conclude that the BF bounds in AdS d on the mass M for (p + 1)-form gauge fields are 22) a result that applies insofar d > p + 2. Notice that this relation, which refers again to the mass term in the Lagrangian, is invariant under the "massive duality" (see, for instance, [42]) between (p + 1)-form and (d − p − 2)-form fields.

Appendix D The Attractor Solutions in Cosmic and Conformal Time
It is instructive to take a look at the attractor solutions of Section 8 in cosmic time, which seem singular for γ = γ in conformal time. In Section 8 we were led to eqs. (8.9), and the first of them, with a suitable choice of integration constant, determines indeed the metric The corresponding expression in cosmic time reads and is regular as λ → ∞, a limit where the Universe evolves in time with no acceleration. Here