Quasi-normal modes of a natural AdS wormhole in Einstein–Born–Infeld Gravity

We study the matter perturbations of a new AdS wormhole in (3+1)\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$(3+1)$$\end{document}-dimensional Einstein–Born–Infeld gravity, called “natural wormhole”, which does not require exotic matters. We discuss the stability of the perturbations by numerically computing the quasi-normal modes (QNMs) of a massive scalar field in the wormhole background. We investigate the dependence of quasi-normal frequencies on the mass of scalar field as well as other parameters of the wormhole. It is found that the perturbations are always stable for the wormhole geometry which has the general relativity (GR) limit when the scalar field mass m satisfies a certain, tachyonic mass bound m2>m∗2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$m^2>m_*^2$$\end{document} with m∗2<0\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$m_*^2<0$$\end{document}, analogous to the Breitenlohner-Freedman (BF) bound in the global-AdS space, mBF2=3Λ/4\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$m_{\mathrm{BF}}^2=3 {\Lambda }/4$$\end{document}. It is also found that the BF-like bound m∗2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$m_*^2$$\end{document} shifts by the changes of the cosmological constant Λ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$${\Lambda }$$\end{document} or angular-momentum number l, with a level crossing between the lowest complex and pure-imaginary modes for zero angular momentum l=0\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$l=0$$\end{document}. Furthermore, it is found that the unstable modes can also have oscillatory parts as well as non-oscillatory parts depending on whether the real and imaginary parts of frequencies are dependent on each other or not, contrary to arguments in the literature. For wormhole geometries which do not have the GR limit, the BF-like bound does not occur and the perturbations are stable for arbitrary tachyonic and non-tachyonic masses, up to a critical mass mc2>0\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$m_{c}^2>0$$\end{document} where the perturbations are completely frozen.


Introduction
Oscillations in closed systems with conserved energies are described by normal modes with real frequencies. Free fields propagating in a confining box correspond to those cases. a e-mail: jykim@kunsan.ac.kr b e-mail: cohlee@gmail.com c e-mail: muinpark@gmail.com On the other hand, in open systems with energy dissipations, oscillations are described by quasi-normal modes (QNMs) with complex frequencies. Perturbations of fields propagating in the background of a black hole correspond to these cases. In the presence of a black hole, the (gravitational or matter) fields can fall into the black hole so that their energies can dissipate into the black holes and the fields decay The complex frequencies of QNMs carry the characteristic properties of a black hole like mass, charge, and angular momentum, independent of the initial perturbations. Because the computational details of QNMs depend much on the based gravity theories, QNMs can reflect the information about the gravity theory itself as well as that of the background spacetime. In the recent detection of gravitational waves by LIGO and VIRGO, which are thought to be radiated from mergers of binary black holes or neutron stars, there is a regime, called ring-down phase, which can be described by QNMs [1,2]. As more precise data be available in the near future, QNMs will be one of the key tools for the test of general relativity (GR) as well as the black hole spacetime [3].
QNMs of black hole systems have been studied for a long time and much have been known in various cases (for some recent reviews, see [4,5]). There is another important system, wormhole spacetime, which corresponds to an open system so that QNMs appear too. Fields entering into a wormhole without return would be also observed as the modes with dissipating energy and decay.
Because the characteristics of the metric near the throat of a wormhole is different from those near the horizon of a black hole, one can distinguish them by comparing their QNMs of the gravitational waves with the same boundary condition at asymptotic infinity. It has been found that wormhole geometries can also show the similar gravitational wave forms as in the black hole systems up to some early ring-down phase but some different wave forms at later times [6,7] (see also [8][9][10][11][12][13] for relevant discussions). In the near future, with increased precisions of gravitational wave detections, it may be possible to distinguish those two systems by investigating their late-time behaviors.
Compared to QNMs in the black hole systems, there are several issues about the wormholes themselves, which are still thought to be some hypothetical objects without any conclusive observational evidence, even though they can be exact solutions of Einstein's equation. In the conventional approaches to construct wormholes, there are the "naturalness problems" due to (i) the hypothetical exotic matters which support the throat of a wormhole but violate energy conditions [14] and (ii) the artificial construction of the wormhole throat by cuts and pastes [15,16]. Actually, in the recent analysis of gravitational waves from wormholes [6,7], the considered wormholes are known as the "thinshell" wormholes which are quite artificial [15,16].
Recently a new type of wormhole solutions was proposed to avoid the problem caused by the exotic matters [17,18]. In the new type of solutions, named as " natural wormholes" [18], the throat is defined as the place where the solutions are smoothly joined. The metric and its derivatives are continuous so that the exotic matters are not introduced at the throat. From the new definition, throat can not be constructed arbitrarily contrary to the conventional cuts and pastes approach. The purpose of this paper is to study QNMs for these natural wormholes.
In this paper, we consider the recently constructed Anti-de Sitter (AdS) wormholes in Einstein-Born-Infeld gravity [19] and compute QNMs of a massive scalar field perturbation in the wormhole background. We consider the asymptotically AdS case since it is simpler than that of the asymptotically flat or de Sitter. Moreover there are several interesting aspects which are absent or unclear in other cases.
For example, it is well known that there exists a tachyonic mass bound, called Breitenlohner-Freedman (BF) bound, m 2 > m 2 BF , for the "conserved and positive" energy of perturbations of a massive scalar field with mass m in the global AdS background [20][21][22][23] (see [24,25] for generalization to higher spins). The solutions exist with discrete real frequencies of ordinary normal modes above the BF bound and the perturbation becomes unstable below the BF bound. What we are going to study in this paper is about what happens in the BF bound for wormholes in the asymptotically AdS spacetime. It would be physically clear that the local deformation of a spacetime by the presence of wormholes would not change the stability properties of the whole spacetime much from the stability property at asymptotic infinity which is governed by the BF bound: It is hard to imagine a smooth spacetime where the (matter) perturbations with m 2 < m 2 BF are partly unstable at infinity but also partly stable near wormholes, by some local effects. This implies that the perturbations of massive fields in the background of AdS wormholes would show both QNMs and BF bound.
We will numerically compute these for a minimally-coupled real scalar field based on the approach of Horowitz and Hubeny for AdS space [26]. Moreover, the asymptotically AdS case would be interesting in the string theory contexts of the AdS/CFT correspondence. QNMs for AdS black hole spacetimes have been much studied in this context [27][28][29][30] but little is known for AdS wormhole spacetimes.
The existence of large charged black holes or wormholes would be questionable since our universe seems to be chargeneutral in the large scales. However in the small scales, the charged black holes or wormholes may exist, as the charged elementary particles do. The well-known charged black hole is Reissner-Nordstrom (RN) black hole with the usual Maxwell's electromagnetic field in GR. But at short distances, we need some modifications of GR for a consistent quantum theory, i.e., (renormalizable) quantum gravity [18]. We may also need modification of Maxwell's electromagnetism as an effective description of quantum effects or genuine classical modifications at short distances. The nonlinear generalization of Maxwell's theory by Born and Infeld (BI) corresponds to the latter case [31,32] and in this set up we may consider the generalized charged black holes and wormholes which include the RN case as the GR limit [33][34][35][36][37][38][39][40][41][42][43][44]. On the other hand, with the advent of D-branes, the BItype action has also attracted renewed interests as an effective description of low energy superstring theory [45,46].
The organization of the paper is as follow. In Sect. 2, we consider the new AdS wormhole in Einstein-Born-Infeld (EBI) gravity. In Sect. 3, we set up a formalism to calculate QNMs of a massive scalar field. In Sect. 4, we set up the formula for numerical computation of QNMs. In Sect. 5, we summarize our numerical results of QNMs. In Sect. 6, we conclude with some discussions. Throughout this paper, we use the conventional units for the speed of light c and the Boltzman's constant k B , c = k B = 1, but keep the Newton's constant G and the Planck's constanth unless stated otherwise.

New AdS wormholes in EBI gravity
In this section, we describe a new AdS wormhole solution in EBI gravity which does not require exotic matters [19]. To this end, we start by considering the EBI gravity action with a cosmological constant in D = 3 + 1 dimensions, where L(F) is the BI Lagrangian density, given by Here, the parameter β is a coupling constant with dimensions [length] −2 which flows to infinity to recover the usual Maxwell's electrodynamics at low energies. Taking 16π G = 1 for simplicity, the equations of motion are obtained as where the energy-momentum tensor for BI fields is given by For the static and spherically symmetric metric ansatz, (6) and the electrically charged case where the only nonvanishing component of the field-strength tensor is F rt ≡ E(r ), the general solution is given by in terms of the hypergeometric function [33][34][35][36][37][38][39][40][41][42][43]. Here Q represents the electric charge located at the origin and M is the ADM mass which is composed of the intrinsic mass C and (finite) self energy of a point charge M 0 , defined by The metric function has the different behavior depending on β Q and ADM mass M (Fig. 1).
In the construction of natural wormholes, the throat which connects two universes (or equivalently, two remote parts of the same universe) is defined as the place where the solutions are smoothly joined. For the reflection (Z 2 ) symmetric universe, the new spherically symmetric wormhole metric is described by when there exits the throat r 0 , defined by and the matching condition, with two coordinate patches, each one covering the range [r 0 , +∞). If there is a singularity-free coordinate patch M + for all values of r ≥ r 0 , one can construct a smooth regular wormhole-like geometry, by joining M + and its mirror patch M − at the throat r 0 . Note that, in this new definition, throats can not be constructed arbitrarily contrary to the conventional cuts and pastes approach. Moreover, in the new approach, f ± (r 0 ) needs not to be vanished in contrast to Morris-Thorne's approach [14], while the quantities d N ± (r 0 )/dr, d f ± (r 0 )/dr in (12) need not to be vanished in both Morris-Thorne's approach [14] and Visser's cuts and pastes approach [15,16].
In Fig. 1 for the solution (7) one can easily see the existence of the throat r 0 satisfying the conditions (12) and (13), depending on the mass M for given values of β, Q, and . Now, from the property of the metric function [33][34][35][36][37][38][39][40][41][42][43] d dr one can find that at the throat r 0 , the largest r of d f/dr = 0, Comparing (15) with the general solution (7), the wormhole mass M can be expressed in terms of r 0 as, which is a monotonically decreasing function of r 0 with the maximum value M 0 of (10) at r 0 = 0 (thick curves in Fig. 2). It is interesting to note that the mass of our new AdS wormhole without exotic matters can be negative for large r 0 , similar to the conventional wormholes which require the exotic matters and violate energy conditions. This may be considered as another evidence that exotic matters cemented at the throat are not mandatory for constructing large scale wormholes.  Fig. 1 The plots of f (r ) for varying M with a fixed β Q (β Q > 1/2 (left), β Q = 1/2 (center), β Q < 1/2 (right)) and a negative cosmological constant < 0 . We consider (top to bottom) Fig. 2 The plots of the ADM mass M vs. the wormhole radius r 0 (thick curves) and the black hole horizon radius r + (thin curves) for varying β Q with a fixed cosmological constant < 0. The marginal mass M 0 is given by the mass value at r 0 or r + = 0. For wormholes, M(r 0 ) is a monotonically decreasing function with the maximum value M 0 at r 0 = 0. For black holes, M(r + ) is a monotonically increasing function with the minimum value M 0 at r + = 0 when β Q ≤ 1/2 (three thin curves from below) and concave with the minimum M * < M 0 at the extremal horizon r * + when β Q > 1/2 (top thin curve). We consider β Q = 2/3, 1/2, 2/4.5, 1/3 (top to bottom) with β = 2 and = −1/5 The wormhole mass (16) is in contrast to the black hole mass M in terms of the black hole horizon r + , corresponding to the largest r of f (r ) = 0, which is positive definite. This is a monotonically increasing function of r + with the minimum M 0 at r + = 0 when β Q ≤ 1/2 so that there exists only the Schwarzschild-like (type I) black hole with one horizon (three thin curves from below in Fig. 2). On the other hand, when β Q > 1/2 (top thin curve in Fig. 2 Fig. 3 The plots of the Hawking temperature T H or f (r 0 )/r 0 vs. the black hole horizon radius r + or the wormhole throat radius r 0 for varying β Q with a fixed cosmological constant < 0. We consider β Q = 2/3, 1/2, 2/4.5, 1/3 (bottom to top curves) with β = 2, = −1/5 one horizon. In this latter case, the black hole mass function (17) is concave with the minimum which is smaller than M 0 , at the "extremal" horizon r * + , where the outer horizon r + meets the inner horizon r − at with the vanishing Hawking temperature for the outer horizon r + (Fig. 3), In the latter case, the wormhole mass M increases as the throat radius r 0 reduces, by accretion of ordinary (positive energy) matters until it reaches to the extremal black hole horizon r * + where the wormhole mass is equal to the black hole mass M(r 0 ) = M(r + ) = M * . Then, no further causal contact with the wormhole is possible "classically" afterwards since the throat is located inside the horizon r + . 1 Hence, for the case β Q > 1/2, the ranges of r 0 and the wormhole mass M(r 0 ) are bounded by r 0 > r * + , M(r 0 ) < M * for the "observable" wormhole throat outside the black hole horizon r + , in contrast to r 0 ≥ 0, M(r 0 ) ≤ M 0 for the former case β Q ≤ 1/2.
Finally we note that, near r 0 , the metric function can be expanded as with the second moments, At large r , on the other hand, the metric function is expanded as

Massive scalar perturbations in the new AdS-EBI wormhole
In this section, we consider the perturbations of a massive scalar field and its QNMs in the new AdS-EBI wormhole background. The wave equation for a minimally-coupled massive scalar field (t, r) with mass m is given by Considering the mode solutions with the spherical harmonics Y (θ, φ) on S 2 , the wave equation reduces to the standard radial equation, where r * is the tortoise coordinate, defined by and V (r ) is the effective potential, given by with the angular-momentum number l.
Choosing the tortoise coordinate r * = 0 at the throat r 0 , one obtains near the throat r ≈ r 0 and at large r , using the asymptotic expansions (21) and (23), respectively. Here, . From the near-throat behavior of the effective potential V , the mode solution near the throat is obtained as where Here, A 1 and A 2 parts represent purely ingoing and outgoing modes, respectively. Since QNMs are defined as solutions which are purely ingoing near the throat, we set A 2 (θ, φ) = 0 as our desired boundary condition at the throat. Here, it is interesting to note that the solutions at the throat are not light-like "generally" due to non-vanishing f (r 0 ) and the effective potential V (r 0 ), in contrast to the always-light-like solutions at the black hole horizon r + , where f (r + ) and the effective potential (28) vanish: The effective potential V (r 0 ) may vanish when the mass of scalar field m satisfies m 2 = −l(l + 1)/r 2 0 (for example, m = 0 for l = 0, or m 2 = −6/r 2 0 for l = 2), but generally it does not 2 (Fig. 4). On the other hand, at r = ∞, which corresponds to a finite value of r * | r =∞ = ∞ r 0 f −1 dr, the effective potential V (r ) diverges as In terms of the tortoise coordinate r * , we have + · · · for the limit r → ∞, from (30). Then, the radial wave equation (26) reduces to where λ ≡ 3 −1 (m 2 − 2 /3) and r * is the shifted tortoise coordinate r * ≡ r * − ∞ r 0 f −1 dr, which approaches zero as r → ∞.
Footnote 2 continued at r 0 but it is negative for r > r 0 , whereas for m 2 ≥ 2 /3, V is positive for the whole region of r ≥ r 0 , otherwise, i.e., for −l(l + 1)/r 2 0 < m 2 < 2 /3, V is not positive definite. It is interesting to note that in the last case V (r 0 ) < 0, the ingoing waves become "tachyonic" at the throat, i.e., k 2 > ω 2 and we will see later that these perturbations are still stable if it is not too much tachyonic, i.e., 2 /3 > m 2 > 3 /4. Now, near r * = 0 (r = ∞), the leading order solution of (36) is obtained as Since the norm of the wave function is given by (37) is squareintegrable only for B 2 = 0 and or equivalently 3 This result agrees also with the condition of regularity or finite energy of the solution [20][21][22][23]47]. In particular, (40) represents the stability condition of massive scalar perturbations in the global AdS space, 4 m 2 > m 2 BF with the BF bound m 2 BF = 3 /4 [20][21][22][23]49]. Moreover, note that the solution (37) with the bound (40), satisfies the vanishing Dirichlet boundary condition at r = ∞ ( r * = 0) even though the effective potential V is not positive infinite (Fig. 4): at r = ∞, V is positive infinite for m 2 > 2 /3 but zero or negative infinite for 2 /3 ≥ m 2 > 3 /4. The usual stability criterion based

Massive Quasi-Normal Modes
QNMs are defined as the solutions which are purely ingoing near the throat ∼ e −i(ωt+kr * ) . In this paper, our interest is the dependence of QNMs on the mass of perturbed fields and in this section we will consider their computations, which are called "massive" QNMs [51], based on the approach of Horowitz and Hubeny (HH) [26]. In order to study QNMs, it is convenient to work with the Eddington-Finkelstein coordinate by introducing the ingoing null coordinate v = t + r * with the metric ds 2 = − f (r )dv 2 + 2dvdr + r 2 (dθ 2 + sin 2 θ dφ 2 ). (41) Considering the mode solution, the wave equation (24) reduces to the radial equation for ϕ(r ), with the reduced effective potential V (r ), Note that, as in the effective potential V (r ), the reduced potential V (r ) is not positive definite and its positivity depends on m 2 (Fig. 5): V (r ) is positive definite for the whole region of r ≥ r 0 only for m 2 > 2 /3.
To compute QNMs, we will expand the solution as a power series around the wormhole throat r 0 and impose the vanishing Dirichlet boundary conditions at r = ∞, following the approach of HH [26]. In order to treat the whole region of interest, r 0 ≤ r < ∞, into a finite region, we introduce a new variable x = 1/r so that the metric (41) becomes 6 The scalar field equation can be written as (46) where x 0 = 1/r 0 and the coefficient functions are given by The overdot (˙) represents the derivative with respects to x.
Since f (x 0 ) > 0 in our wormhole system, one can remove the overall (x − x 0 ) −1 factor in (46) so that x = x 0 is not a singular point, whereas there is one regular singular point at the spatial infinity x = 0. Then one can expand Eq. (46) around the throat x 0 up to the pole at x = 0 and solve the equation at each order of the expansion. First, expanding s, t, u around x = x 0 as one can obtain the first few coefficients of them as follows, where we have usedḟ (x 0 ) = 0 and with the second moments σ = (d 2 f /dr 2 )| r 0 given by (22). 7 Now in order to consider the expansion of the solution around the throat r 0 , we first set ϕ = (x − x 0 ) α as the lowest order solutions. Then, at the leading order n = −1, one obtains the indicial equation, which gives two solutions, α = 0 and α = 1. The first solution, α = 0, corresponds to the ingoing mode ∼ e −iωv near the throat. The second solution, α = 1, is also an ingoing mode near the throat but vanishing at the throat as ∼ e −iωv (x − x 0 ). Since in this paper we want to consider nonvanishing ingoing modes to study QNMs, we take only the α = 0 case. 8 Then the desired solution can be expanded as 7 For the black hole cases, the coefficients are obtained as s 0 = 2κ x 2 (49), the most important qualitative difference is the absence of s −1 in the black hole case so that the horizon x + = 1/r + becomes a regular singular point. Other coefficients look similar, with the role of the surface gravity κ at the black hole horizon replaced by x 0 f (x 0 ) in our natural wormhole case: this may be understood from the direct relation x 0 f (x 0 ) = 2κ| r+→r0 = 4π T H | r+→r0 in (14). 8 The α = 1 case corresponds to normal modes without any wave flow, i.e., energy loss at the throat. It is interesting that our wormhole system allows also this solution as well as QNMs with the ingoing mode solutions of α = 0. This is in contrast to the black hole system, where outgoing mode solutions are allowed instead, as well as the ingoing modes at the horizon.
Plugging (52) into (46) with the expansion (48), one obtains the recursion relation for a n (n = 0, 1) as follows: where Generally we can get two parameter families of solutions in terms of a 0 and a 1 near x = x 0 . As we have discussed already, a 0 term corresponds to a pure ingoing mode at x = x 0 so that a 0 should be kept and in this paper we set a 0 = 1 for convenience. On the other hand, a 1 term corresponds to a vanishing ingoing mode at x = x 0 so that we may discard this family of solution, which actually satisfies the additional Neumann boundary condition for ϕ, i.e., ϕ | x 0 = a 1 ≡ 0. In this paper, we are only interested in this case for simplicity. As r → ∞, (46) reduces to which leads to the asymptotic solution as corresponding to the solution in (37). Since we are interested in the normalizable modes, we take C 2 = 0 and the desired solution is ϕ(r ) ∼ r − 1 2 (1+ √ 9−12m 2 / ) , which also satisfies the vanishing Dirichlet boundary condition ϕ(r ) → 0 as r → ∞ (x → 0). This means that we impose the boundary condition as an algebraic equation at x = 0, which is satisfied only for some discrete values of ω since a n 's are functions of ω from (53). If the sum (57) is convergent, one can truncate the summation at some large order n = N where the partial sum beyond n = N does not change within the desired precision. Because this approach can easily be implemented numerically, particularly in Mathematica, the coefficients a n , s n , t n , u n can be computed up to an arbitrary order N . In the next section, we present the numerical computation of QNM frequencies ω ≡ ω R − iω I based on this method.

Numerical results and their interpretations
In this section, we will show the results of numerical computation of QNMs as described in the previous section. In this paper, we consider only the "lowest" QNMs, whose absolute magnitude, |ω| = ω 2 R + ω 2 I , is the smallest, unless stated otherwise. First of all, Figs. 6 and 7 show the lowest QNM frequency ω = ω R − iω I as a function of m 2 for varying M and Q. Here, we focus on the case of β Q > 1/2, where the well-defined GR limit of β → ∞ exists [19]. The result shows that the perturbations are stable (ω I > 0) if m 2 is above certain threshold values m 2 * (−0.16769, −0.16720, −0.16704 for M = 10 −5 , 0.1, 0.15 with Q = 1 (Fig. 6); −0.16769, −0.16728, −0.16704 for Q = 1, 0.9, 0.85 with M = 10 −5 (Fig. 7)). For a given value of M or Q, QNM frequencies ω I and ω R increase as m 2 increases above m 2 * . Here, we note that the critical mass m 2 * is close to the BF bound of (40), m 2 BF = −3 /4 = −0.15 [20][21][22][23]. On the other hand, for a given value of m 2 , ω I and ω R increase as M decreases or Q increases, corresponding to increasing throat radius r 0 from (16) (Fig. 2). Neglecting the small differences of m 2 * for different M and Q, we may approximately fit the numerical result of the m 2 dependence in Figs. 6 and 7 to the analytic functions near the critical mass squared m 2 * , with the approprite coefficients, b n and c n (n = 1, 2, . . . ).  Figure 9 shows the lowest QNM frequency as a function of m 2 for varying angular-momentum number l. The result shows that the critical mass shifts as m 2 * ≈ −0.16769, −0.16679, −0.15524 for l = 2, 1, 0, respectively. Especially for l = 0, it shows a level crossing between the lowest pure-imaginary mode representing an over-damping (purple color) and the lowest complex mode (pink color) at m 2 ≈ −0.1089 before the critical mass m 2 * is being reached, so that the instability is governed by the used-to-be higher (pure) imaginary frequency modes. 9 On the other hand, there When l = 0, it shows a level crossing between the lowest pureimaginary mode (purple color) and the lowest complex mode (pink color) at m 2 ≈ −0.1089 before the on-set of instability is being reached. Moreover, there are discontinuities in ω I and ω R for the lowest ω = ω R −iω I (green color) at m 2 ≈ −0.0784 before the level-crossing point are discontinuities in ω I and ω R at m 2 ≈ −0.0784 for the lowest complex frequency ω = ω R − iω I (green color) even before the level-crossing point. 10 Figure 10 shows the QNM frequency as a function of l for varying m 2 . For small l (l ≤ 5), ω I decreases but ω R increases (except for the case m 2 < 0) as l increases, whereas for large l, both ω I and ω R increase as l increases. It is interesting to note that there is a bouncing point of ω I , where ω I = 0 at l = 5. Here we have considered only the case m 2 > m 2 * , which is stable for small l. Figure 11 shows the QNM frequency as a function of r 0 for varying m 2 in Fig. 6. Though the result is preliminary Footnote 9 continued is increased generally. It would be interesting to check whether other unstable branches exist for higher modes but this is beyond the scope of this paper. 10 For the level crossings in black strings, where the effective masses due to Kaluza-Klein reduction is naturally introduced, see [52]. It seems this phenomena is universal in massive QNMs. since there are only limited data points, i.e., for a given value of m, only three points of r 0 which correspond to the three values of M in Fig. 6, the result indicates interestingly the linear dependence of QNM frequency to the throat radius.
Explicitly, the curves can be fitted to tively. This is similar to the case for large black holes where QNM frequency depends linearly on the horizon radius (ω I , ω R ∝ r + ) [26][27][28][29]. 11 11 Since the quantity f (r 0 )/r 0 , which is given by − r 0 + 1/r 0 − Q 2 /r 3 0 + Q 4 /4β 2 r 7 0 + O(r −11 0 ), corresponds to the surface gravity for black hole case, 2κ = 4π T H = (d f (r )/dr)| r+ , as noted in footnote No. 7, the wormhole's QNM frequencies (59) may also be fitted  The asymptotic linear dependence can also be understood as the result of the scaling behavior [26,53,54], 12 by which the perturbation equation (46) is unchanged. This means that the QNM frequency ω = ω R − iω I , which is a function of r 0 , , Q, β, and m, should have the following form in order to have the scaling ω → ω/α. For large r 0 , the dominant terms are given by ω ≈ζ r 0 +ηβ + δ m 2 +γ −1 m 4 + · · · r 0 , 12 The scaling for the (abbreviated) wormhole mass M, which differs from that of scalar field mass m, is due to the omitted Newton's constant whereζ ,η,δ, andγ are scale invariant coefficients, which agrees with the behavior of (59). 13 So far, we have studied the case β Q > 1/2, which has a well-defined GR limit at β → ∞. Now, we show in Fig. 12 the case β Q ≤ 1/2, which do not have a GR limit. The result shows that there is no oscillatory part (ω R = 0) and moreover the critical mass squared m 2 * < 0 does not occur in this case. Rather, it shows another critical mass squared m 2 c ≈ 1.0326 for β Q < 1/2 so that the perturbations would be completely "frozen", i.e., ω = ω R − iω I = 0, for m 2 > m 2 c . Even though this result could be preliminary too since we may not neglect the back reaction of the wormhole geometry for the heavy-mass perturbations [55,56], 14 it seems to agree with the so-called "quasi-resonance modes (QRMs)" with ω I = 0 in massive QNMs, though the oscillatory parts are different, i.e., ω R = 0 in our wormhole case but ω R = 0 in QRMs [51]. 13 Expanding near the critical mass squared m 2 * and comparing with (58), one can obtain the relationsζ Before finishing this section, we end up with some remarks about the consistency of our numerical results. First, Fig. 13 shows the truncated wave function ϕ N (x), reconstructed from the numerically obtained a n 's in (52) up to the order N = 300. These show the vanishing Dirichlet boundary condition (ϕ(x) → 0) as x → 0 and the vanishing Neumann boundary condition (dϕ/dx → 0) as x → x 0 from our choice of α = 1 in the indicial equation (51). Moreover, the asymptotic behavior of our desired wave function ϕ(x) ∼  (56), whose exponent can be captured by x ln(dϕ/dx) → 1 2 (1 + 9 − 12m 2 / ) as x → 0, which are computed as 2, 2.39737, 1.44868, 1.05317, 0.78983 for m 2 = 0, 0.09, −0.09, −0.1296, −0.1444, is well confirmed by the numerically reconstructed wave function. 15 Second, for the unstable modes (ω I < 0) beyond the critical mass m 2 < m 2 * , Figs. 8 and 9 show that there exits the oscillation mode with the non-vanishing ω R which is continuously changing across the on-set point of the instability ( = −0.13, −0.1 case (l = 2) in Fig. 8 and l = 1 case ( = −0.2) in Fig. 9). But for some cases ω R vanishes with a sudden discontinuity before the on-set point of instability is being reached (l = 0 case ( = −0.2) in Fig. 9). This seems to contradict the argument in the literature which claims that " ω R = 0 for the unstable mode, ω I < 0 ", though there is no restriction on ω R for the stable mode, ω I > 0 [52,57]. In order to clarify this issue, we consider the integral,   Fig. 8 with varying < 0 (l = 2) (left), and in Fig. 9 with varying l ( = −0.2) (right). The left shows a smooth non-vanishing function ω R = ω R (ω I ) across the instability point for = −0.13 (blue) and = −0.1 (green). The right shows the vanishing ω R for the unstable region (ω I < 0) with non-smooth transitions before the instability point for l = 1 (blue) and l = 0 (green). The red curve is the case = −0.2 (l = 2) in Figs. 8 and 9 shows also the smooth ω R = ω R (ω I ) across the instability point though it is not quite clear in the plot ω R as a function of ω I , ω R = ω R (ω I ), (67) is generally a non-linear equation for one independent variable ω I and its solution needs not to agree with the previous naive one without separating independent variables, which may lead to misleading solutions. This means that ω R = 0, ω I < 0 (oscillating, unstable modes) can also be the possible solution As m 2 becomes negatively larger, N needs to be higher to achieve the convergence and these cases are not included in this paper depending on the details of ω R = ω R (ω I ). Actually, Fig. 14 shows the relation ω R ≈ 1/2+a ω I +b ω 2 I · · · which allows the continuous solution of ω R = 0, ω I < 0, as implied by the result of (58) (left), as well as the usual discontinuous solution (right, l = 0, 1 case). This indicates the existence of more fundamental reason for the relation. 18 The usual result ω R = 0, ω I < 0 for the case l = 0 may be due to the independence of ω I (< 0) from ω R after the level crossing of two initially different modes.
Finally, in order to obtain reliable numerical results we need to compute the partial sum with the typical truncation of the order of N = 250 (Fig. 15). In this work, we consider up to N = 300 for most computations, but we consider up to N = 400 for the level crossing of l = 0 QNMs in Fig. 9.

Concluding remarks
We have studied QNMs for a massive scalar field in the background of a natural AdS wormhole in EBI gravity, which has been recently constructed without exotic matters. For the case where the GR limit exists, i.e., β Q > 1/2, we − d 2 d r 2 * + 1 4 ω 2 r 2 * + ξ r * − λ r 2 * − E ϕ = 0 (68) with the energy E and it would be interesting to study its connection to some integrable theories at the boundary.
As the final remark, it would be straightforward to extend our formalism to more general perturbations with spins, including the (gravitational, spin 2) perturbations of the wormhole space-time itself. It would be interesting to study whether ring-down phases of natural wormholes can mimic those of black holes.