On perturbation theory and critical exponents for self-similar systems

Gravitational critical collapse in the Einstein-axion-dilaton system is known to lead to continuous self-similar solutions characterized by the Choptuik critical exponent γ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\gamma $$\end{document}. We complete the existing literature on the subject by computing the linear perturbation equations in the case where the axion-dilaton system assumes a parabolic form. Next, we solve the perturbation equations in a newly discovered self-similar solution in the hyperbolic case, which allows us to extract the Choptuik exponent. Our main result is that this exponent depends not only on the dimensions of spacetime but also the particular ansatz and the critical solutions that one started with.


Introduction
A well-known property of black holes as the end state of gravitational collapse is that they are completely defined by only three numbers: their mass, angular momentum, and charge. Choptuik revealed in [1] that there may be a fourth universal quantity characterizing the collapse itself. Following the study of Christodolou in [2][3][4] on the spherically symmetric collapse of scalar fields, Choptuik discovered a critical behavior illustrating some sort of discrete spacetime selfsimilarity. Expressing the amplitude of the scalar field fluctuation by the number p, he found that p should exceed a critical value p crit in order to form a black hole. Furthermore, for values of p above the threshold, the mass of the black hole M bh (equivalently, its Schwarzschild radius r S ) exhibits the scaling law where the Choptuik exponent was found to be γ 0.37 [1,5,6] in 4d for a single real scalar field. Note that in general dimensions (d ≥ 4) the definitions get changed [7,8] Along the same lines, diverse numerical simulations with different matter fields have been carried out [9][10][11][12][13][14]. For example the critical collapse of a perfect fluid was performed in [7,[15][16][17]. In [16] the authors found γ 0.36 and hence it was conjectured in [18] that γ may be universal for any matter field that is coupled to four dimensional gravity. Later on, in [7,17,19] it was discovered that the Choptuik exponent can be explored by dealing with perturbations of the self-similar solutions. In order to do so, one needs to perturb any field h (be it the metric or the matter content) as follows where the perturbation h −κ has scaling −κ ∈ C which labels the different modes. Among the allowed values of κ, we define the most relevant mode κ * as the highest value of Re(κ). 1 It was shown in [7,17,19] that κ * is related to the Choptuik exponent by In [20] the case of axial symmetry had been studied and the critical collapse in the presence of shock waves was reviewed in [21]. The case of axion-dilaton critical collapse coupled to gravity in four dimension was first examined in [22] which found the value γ 0.2641, hence raising serious doubts concerning the universality of γ in four dimensions.
One motivation to study critical collapse in the axiondilaton system is the AdS/CFT correspondence [23][24][25][26], relating Choptuik exponent, the imaginary part of quasinormal modes, and the dual conformal field theory [27]. Other motivations include the holographic description of black hole formation [8] as well as the physics of black holes and its applications [28]. In type IIB string theory one is often interested in exploring the gravitational collapse on spaces that can asymptotically approach to Ad S 5 × S 5 where the matter content is described by the axion-dilaton system and the self-dual 5-form field.
The entire families of distinguishable continuous self similar solutions of the Einstein-axion-dilaton system in four and five dimensions for all the three conjugacy classes of SL(2, R) were recently explored in [31] that generalized the previous efforts done in [32,33]. Based on some robust analytic and numerical techniques in [34], we did perturb critical solution of four-dimensional elliptic critical collapse and were able to recover the known value [22] of γ ∼ 0.2641. Hence this provides strong confidence in our ability to obtain the other critical exponents in different dimensions as well as for different classes of solutions.
In this article, after a brief recap on self-similar solutions to the Einstein-axion-dilaton system, we set up a linear perturbation analysis which will allow us to extract the Choptuik exponent in any dimensions. The new methodology that we employ is quite generic and could be applied to other matter contents as well. Using this framework, we derive the perturbation equations in all conjugacy classes of SL(2, R), and particularly in the parabolic case which was not studied before. We extract the Choptuik exponent in a new branch of the 4d hyperbolic class of solutions and find that its value is different from the other branches of solutions. Thus, our results cast doubts concerning the universality of the Choptuik exponent.

Self-similar solutions to Einstein-axion-dilaton configuration
The Einstein-axion-dilaton system that coupled to gravity in d dimensions is defined by the following action that can be described by the effective action of type II string theory [35,36] where the axion-dilaton is defined by τ ≡ a + ie −φ . This action enjoys the SL(2, R) symmetry where α, β, γ , δ are real parameters satisfying αδ − βγ = 1. It was known that once quantum effects are taken into account the SL(2, R) symmetry does reduce to SL(2, Z) and this Sduality was also believed to be a non-perturbative symmetry of IIB string theory [37][38][39]. Now from the above action one can read off the equations of motion We assume spherical symmetry on both background and perturbations so that the general form of the metric in d dimensions is where d 2 q is the angular part of the metric in d spacetime dimensions. A scale invariant solution is found by requiring that under a spacetime dilation (or scale transformation), (t, r ) → ( t, r ), the line element gets changed as ds 2 → 2 ds 2 . Thus, the metric functions should be scale invariant, i.e. u(t, r ) = u(z), b(t, r ) = b(z), z ≡ −r/t. Since the action (5) is invariant under the SL(2, R) transformation (6), τ only needs to be invariant and up to an SL(2, R) transformation, We call a system of (g, τ ) respecting the above properties a continuous self-similar (CSS) solution. Note that different cases do relate to various classes of dM d =1 [31], so that τ can take three different forms, where ω is an unknown real parameter and the function f (z) must satisfy | f (z)| < 1 for the elliptic case and Im f (z) > 0 for the other two cases. Note that one can show that the the ansatz τ (t, r ) = (−t) ω f (z) also leads to the same equations of motion for hyperbolic case (it is simply a conformal transformation of τ ). If we replace the CSS ansätze in the equations of motion we then get a differential system of equations for u(z), b(z), f (z). Due to spherical symmetry one can show that u(z) can be expressed in terms of b(z) and f (z) so that eventually we are left out with some ordinary differential equations (ODEs) The above equations have five singularities [32] located at z = ±0, z = ∞ and z = z ± where the last singularities are defined by b(z ± ) = ±z ± . The latter correspond to the homothetic horizon and it can be shown that z = z + is just a mere coordinate singularity [22,32], hence τ is regular across it which translates back to the finiteness of f (z) as z → z + . Now one may observe that the vanishing of the divergent part of f (z) gives us a complex valued constraint at z + which we denote by where the explicit form of G was given in [31]. Using regularity at z = 0 and some residual symmetries one obtains the initial conditions b Here x 0 is a real parameter. Hence, we have two constraints (the vanishing of the real and imaginary parts of G) and two parameters (ω, x 0 ). The discrete solutions in four and five dimensions were found in [34]. These solutions are constructed by integrating numerically the equations of motion. For instance, for the four dimensional elliptic case just one solution is determined [32,40] as To deal with self-similar solutions for parabolic cases, the following remarks are in order. First, we have an additional symmetry as follows then τ also transforms as τ → K τ , which means that if (ω, Im f (0)) is a solution, so is (K ω, K Im f (0)). The reason behind it is that all equations of motion and the constraint G(ω, Im f (0)) are invariant under this new scaling. Therefore, the only real unknown parameter for parabolic class is the ratio ω/Im f (0). We then need to look for the zeroes of G(ω, Im f (0)) for only a real parameter ω/Im f (0). Hence we just set Im f (0) = 1. For the five dimensional parabolic case, we draw below the plot of the zeroes of the real and imaginary parts of G(ω, 1). From Fig. 1 in five dimensions we might note to the tiny value of |G| for a specific value of ω. This may be related to the only possible solution ray, but numerical accuracy is insufficient to assess it with certainty. It is given by Note that remarks about the higher dimensional parbolic solutions are given in [41]. On the other hand three different solutions for the hyperbolic case in four dimensions were  determined in [34]. These three solutions denoted by α, β and γ are summarized in Table 1.
Making use of the root-finding procedure, we also identify a fourth solution δ for the four-dimensional hyperbolic class (with accuracy less than the other solutions and G ∼ 10 −5 ) whose parameters are given by where the graphical representation can be seen in [41].

Perturbative analysis
Here we derive the perturbation equations in general dimensions. We will apply our method for the parabolic case, but it could be taken as an extensive method which holds for all matter content as well. Note that we have taken some of the steps from [42] while with some algebraic calculations we are able to remove u(t, r ) and its derivative from the actual computations. 2 We perturb the exact solutions h 0 (where h denotes either b, u or f ) found in Sect. 2 according to where ε is a small number. If we expand all the equations in powers of ε, then the zeroth order part gives rise to background equations already studied in Sect. 2 and the linearized equations for the perturbations h 1 (t, r ) are related to linear terms in ε. Let us consider the perturbations of the form One finds the spectrum of κ by solving the equations for h 1 (z) and indeed the general solution to the first-order equations is obtained with the linear combination of these modes. We want to find the mode κ * with largest real part (assuming a growing mode for t → 0, i.e Reκ > 0) that is related to the Choptuik exponent by [7,17,19] Note that just like the four dimensional elliptic case, for simplicity we consider only real modes κ * . It can be shown that the values κ = 0 and κ = 1 are gauge modes with respect to global U (1) re-definitions of f and time translations respectively, see Section 3.1.1 of [34]. These modes should be excluded from the computations.

Linearized equations of motion in any dimension for the parabolic class
Let us apply this program to the parabolic case and explore all the linearized perturbations in arbitrary dimension d = q + 2 ≥ 4. One applies the perturbation ansatz (21) to all the functions u, b, τ as One calculates the Ricci tensor for the following metric where b and u should be replaced by the perturbed quantities (23), (24). The zeroth-order and first-order parts of the Ricci tensor are obtained from Likewise one does the same for the matter content, applying the axion-dilaton perturbations (25), (26) so that The Einstein field equations should be held order by order hence We now use some of the above equations to remove u(t, r ) and its derivatives from the other equations. Indeed by using R tr =T (1) tr also removes u 1 (z), where eventually R (1) i j =T (1) i j = 0 is used to actually remove u 1 (z). From now on we also remove the z argument of all functions, so that Since the final form of u 1 (z) is complicated we will not write it here. Therefore, u 0 , u 0 , u 1 , u 1 are completely expressed for all equations in terms of other functions. Using the following combination of temporal and radial equations of motion we also remove the first derivative terms in b(t, r ). Indeed we recover the zeroth-order equation as follows where the overbar on f 0 denotes complex conjugation. In the same way the first correction is defined by which is an equation relating b 1 to b 0 , b 0 f 0 , f 0 , f 0 , and to the other perturbations b 1 , f 1 , f 1 , and which is really linear in all perturbations. In the parabolic case this equation takes the following form with The perturbations are also scale invariant, thus making the coordinate change (t, r ) → (t, z), the factors of t cancels out. We now introduce the perturbation ansätze in the τ equation of motion (8). Replacing b 0 according to (37) and solving for f 0 , one recovers the second order background equation for f 0 , Going to first order, the linearized equation for f 1 is where . This equation is also scale-invariant. By integrating numerically the unperturbed equations, and also substituting b 1 from Eq. (39) , we derive the ordinary linear differential equations as follows B 1 and F 1 are indeed functions linear in the perturbations that have however non-linear dependence on the unperturbed solution. The perturbed equations are also singular at z = 0 and b 2 (z) = z 2 . The perturbation equations for hyperbolic case were derived in [34] where the modes are explored by finding the κ values that are related to smooth solutions of the perturbed equations (43), (44) which need to satisfy the appropriate boundary conditions, which we will now discuss.

Boundary conditions for perturbations
We now turn to boundary conditions needed to solve Eqs. (43), (44). First of all at z = 0 we rescale the time coordinate, so that b 1 (0) = 0, and also using the regularity condition for the axion-dilaton at z = 0 we find that f 1 (0) = 0 so that the freedom in f is reduced to f 1 (0) which is an unknown complex parameter. We also demand that at z + (we recall that z + is defined by the equation b(z + ) = z + ) all equations and perturbations be regular so that all the sec- r ) should be finite as z → z + . Hence, f 0 (z) and f 1 (z) are also finite as z → z + . For brevity, we introduce β = b 0 (z) − z and rewrite Eqs. (42)-(41) as follows where it is understood that h 0 = (b 0 (z + ), f 0 (z + ), f 0 (z + )), ). The vanishing unperturbed Finally we solve this constraint for f 1 (z + ) in terms of f 1 (z + ), b 1 (z + ), κ and h 0 . Thus this condition does reduce the free parameters at z + to just a real number b 1 (z + ) and a complex f 1 (z + ). Finally we will have 6 unknowns including κ and the following five-component vector:   We also have the linear ODE's Eqs. (43), (44) whose total real order is five. Let us now briefly explain the numerical procedure. Given a set of boundary conditions X , we integrate from z = 0 to an intermediate point z mid and similarly we integrate backwards from z + to z mid . Finally we collect the values of all functions (b 1 , Re f 1 , Im f 1 , Re f 1 , Im f 1 ) at z mid and encode the difference between the two integrations in a "difference function" D(κ; X ). By definition, D(κ; X ) is linear in X thus it has a representation as a matrix form where A(κ) is a 5×5 real matrix depending on κ. So we need to just find the zeroes of D(κ; X ) and this can be achieved by evaluating det A(κ) = 0. We carry out the root search for the determinant as a function of κ where the root with the biggest value will be related to the Choptuik exponent through Eq. (22). It is worth highlighting one last point: the perturbed equations of motion are singular whenever the fac- b 0 in the denominator vanishes, so that the numerical procedure fails at particular point. We can get an estimate for the values of κ giving rise to this singular behaviour as follows, However, this apparent problem does not affect our evaluation of the critical exponent because in most cases the most relevant mode κ * lies outside that particular failure region.

Results
In [34] we had already tested the above techniques and were able to derive the critical exponent for the unique four-dimensional elliptic solution. For completeness we have drawn the behaviours of det A(κ) near the last crossing of the horizontal axis in Fig. 2. The position of the crossing is found to be κ * 4E ≈ 3.7858, that gives rise to the Choptuik exponent γ 4E ≈ 0.2641 which is in agreement with [40]. Notice that for this solution, κ sing = 1.224, and the integration fails around 1 κ 1.4, which is well below the location of the most relevant mode as it is seen in a range of κ values in Fig. 2, where Mathematica was not able to complete the computation of det A.
In the 4d hyperbolic case, there are four branches of solutions that we denote by 4H α, 4Hβ, 4H γ and 4H δ respectively. The Choptuik exponent was not known in the 4H δ case, which is one of the new results of this article. In Fig. 3 we plot the behaviour of det A(κ) near the last crossing which defines the most relevant mode, so that the Choptuik exponent is which is different from the Choptuik exponent for the third critical solution γ 4H γ = 0.436 (already found in [34]) that is illustrated in Fig. 5. We collect these results in Table 2.
For completeness, we include some other Choptuik exponents in Table 3. We refer the reader to [34] for a complete discussion of these other cases.

Conclusion
In this article, we have obtained the linear perturbation equations in all classes of solutions of the self-similar collapse solution to the Einstein-axion-dilaton system, including the parabolic case which was not studied previously. The method which we employ is quite generic and could be applied to any matter content in arbitrary dimensions as well. This is certainly a path that we intend to follow in the future.
Through a numerical procedure, we have obtained the fastest growing mode of the perturbations that determine the Choptuik exponent. We have applied this methodology to a particular branch of solutions whose Choptuik exponent was still unknown. Interestingly, we revealed that not only the Choptuik exponent does depend on the spacetime dimension but also it depends on matter content (which is composed of an axion-dilaton system in this case) as well as the different branches of solutions of self-similar critical collapse. Hence, one may conclude that the original conjecture about the universality of Choptuik exponent is not satisfied. However, there might actually exist some universal behaviours hidden in combinations of critical exponents and various other parameters of the theory which have not been taken into account by our current efforts.

Data Availability Statement
This manuscript has no associated data or the data will not be deposited. [Authors' comment: All data generated or analyzed during this study included in this published article and some data produced by Mathematica software.] Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecomm ons.org/licenses/by/4.0/. Funded by SCOAP 3 .