Quasinormal modes in the field of a dyon-like dilatonic black hole

Quasinormal modes of massless test scalar field in the background of gravitational field for a non-extremal dilatonic dyonic black hole are explored. The dyon-like black hole solution is considered in the gravitational $4d$ model involving two scalar fields and two 2-forms. It is governed by two 2-dimensional dilatonic coupling vectors $\vec{\lambda}_i$ obeying $\vec{\lambda}_i (\vec{\lambda}_1 + \vec{\lambda}_2)>0$, $i =1,2$. The first law of black hole thermodynamics is given and the Smarr relation is verified. Quasinormal modes for a massless scalar (test) field in the eikonal approximation are obtained and analysed. These modes depend upon a dimensionless parameter $a$ ($0<a \leq 2$) which is a function of $\vec{\lambda}_i$. For limiting strong ($a = +0$) and weak ($a = 2$) coupling cases, they coincide with the well-known results for the Schwarzschild and Reissner-Nordstr\"om solutions. It is shown that the Hod conjecture, connecting the damping rate and the Hawking temperature, is satisfied for $0<a \leq 1$ and all allowed values of parameters.


Introduction
The recent discovery/detection of gravitational waves [1][2][3] has strengthen a long-living interest to quasinormal modes (QNMs) [4][5][6][7][8][9][10][11][12][13], predicted by Vishveshwara in 1970. The detected gravitational waves were emitted during the final (ringdown) stage of binary black hole mergers. The frequencies of these waves were governed by a certain superpositions of decaying oscillations, i.e. QNMs. The careful analysis of these experiments may be rather important since it can shed some light on nature of gravity in a strong field regime. a e-mail: algis_malybayev@mail.ru b e-mail: kuantay@mail.ru c e-mail: ivashchuk@mail.ru From the mathematical point of view, the quasinormal mode (QNM) problem can be reduced to studying the solutions to a wave equation for a scalar function Φ(t, x) chosen in the following form where Φ * = Φ * (x) obeys a Schrödinger-type equation defined on a certain domain of real line R = (−∞, +∞), where ε > 0 is some parameter, e.g. ε = 1; for reviews see [10][11][12][13]. For asymptotically flat black-hole solutions the functions Φ * (x) are defined on R. In this case x is chosen as a socalled tortoise coordinate (in the body of the paper denoted as R * ), and (at least) for certain known spherically symmetric solutions (e.g. Schwarzschild and Reissner-Nordström ones) the potential V (x) is a positively defined smooth function, having sufficiently fast fall off (to zero) in approaching either to the horizon (x → −∞) or to the spatial infinity (x → +∞). Usually QNM frequencies ω are defined as complex numbers obeying Re ω > 0 and Im ω < 0, such that the wave functions (1) are exponentially damped in time as (t → +∞), corresponding to asymptotically stable perturbations. The QNM frequencies appear for the solutions to equation (2) which behave as outgoing waves at spatial infinity: Φ * (x) ∼ e iωx ε for x → ∞ (Re ω > 0) and ingoing ones at the horizon: Φ * (x) ∼ e − iωx ε for x → −∞ with exponential growth (in |x|) for |Φ * (x)| as |x| → ∞ (due to Im ω < 0).
For calculation of QNM [12,13] there exists a (most popular) method, introduced in Refs. [7][8][9], which may be called as analytical continuation method. The most transparent version of this method was recently proposed (and verified) in Ref. [14]. Here we consider for simplicity the case of the potential defined on all real axis R = (−∞, +∞) to avoid the boundary problems. (For more involved and subtle case when the Schrödinger operator and effective potential are defined on (0, +∞) and proper boundary condition should be specified see Ref. [15].) The prescription is as follows: one should start with the Schrödinger equation for non-relativistic quantum particle (of mass 1/2) moving in the inverted potential −V (x): where Ψ = Ψ (x) is the wave function. For a potential under consideration the inverted potential −V (x) may have certain bounded states described by discrete spectrum energy levels  [14] tells us that QNM frequencies for the potential V (x) may be obtained from bounded states for the inverted potential −V (x) by putting formallyh = iε in (2). Hence, due to this prescription we get the following QNM frequencies where n = 0, 1, . . . is called as (QNM) overtone number. It should be noted, that the method suggested in Ref. [14] for computation quasinormal frequencies of spherically symmetric black holes, relates them to bound state energies of anharmonic oscillators by using the analytic continuation inh. It was stated in Ref. [14], that the known WKB results are easily reproduced by this method and, moreover, "the perturbative WKB series of the quasinormal frequencies turn out to be Borel summable divergent series both for the Schwarzschild and for the Reissner-Nordström black holes.
Here we study QNM spectrum in eikonal approximation for a special dyon-like dilatonic black hole solution from Ref.
The relation between the 2-forms and color charges are given by where τ 2 = vol[S 2 ] is magnetic 2-form, which is volume form on 2-dimensional sphere and τ 1 is an "electric" 2-form. We note that in the case of one scalar field ϕ and two coupling constants λ 1 , λ 2 the dyon-like ansatz was considered recently in Refs. [17,18,28,29]. For λ 1 = λ 2 = λ our solutions from Ref. [17] were dealing with a trivial noncomposite generalization of dilatonic dyon black hole solutions in the model with one 2-form and one scalar field which was considered in Ref. [16], see also Refs. [24][25][26][27], and references therein.
The solutions with one scalar field from Refs. [17,18] may be embedded to the solutions under examination by considering the case of collinear dilatonic coupling vectors: where e 2 = 1, λ 1 + λ 2 = 0. The paper is organised as follows: in section 2 we review the main properties of the black hole dyon solution from Ref. [30]. In section 3 we consider the physical parameters and particular cases of the dyonic black hole solutions. In section 4 we analytically derive the eikonal approximation for frequences of QNM corresponding to massless test scalar field in the background metric of our dyonic-like black hole solution and study their features. In section 5 we consider two limiting cases a = +0 and a = 2, corresponding to the Schwarzschild and Reissner-Nordström black hole solutions. In section 6 we test/check the validity of the Hod conjecture [40] for the solution under consideration when 0 < a ≤ 2. Finally, we summarize our conclusion in section 7.

Black hole dyon solutions
The action of a model containing two scalar fields, 2-form and dilatonic coupling vectors which was considered in Ref.
Here and in what follows we put c = 1 (where c is the speed of light in vacuum.) We consider a dyonic-like black hole solution to the field equations corresponding to the action (7) which has the following form [30] where Q 1 and Q 2 are (color) charges -electric and magnetic, respectively, µ > 0 is the extremality parameter, dΩ 2 = dθ 2 + sin 2 θ dφ 2 is the canonical metric on the unit sphere S 2 (0 < θ < π, 0 < φ < 2π), τ = sin θ dθ ∧ dφ is the standard volume form on S 2 , with P > 0 obeying All the rest parameters of the solution are defined as follows i = 1, 2 and Here the following additional restrictions on dilatonic coupling vectors are imposed Correspondingly, we note that is valid for λ 1 = − λ 2 . Due to relations (18) and (19) the Q 2 s are well-defined. Note that the restrictions (18) imply relations λ s = 0, s = 1, 2, and (8).
Indeed, in this case we have the sum of two non-negative terms in (16): ( λ 1 + λ 2 ) 2 > 0 and due to the Cauchy-Schwarz inequality. Moreover, C = 0 if and only if vectors λ 1 and λ 2 are collinear. Relation (20) implies For non-collinear vectors λ 1 and λ 2 we get 0 < a < 2 while a = 2 for collinear ones. This solution may be verified just by a straightforward substitution into the equations of motion.
The calculation of scalar curvature for the metric ds 2 = g µν dx µ dx ν in (9) yields

Particular cases and physical parameters
Here we analyze certain cases and physical parameters corresponding to the solutions under consideration.

Non-collinear and collinear cases
Non-collinear case. For non-collinear vectors λ 1 and λ 2 (0 < a < 2) we obtain as R → +0 and hence we have a black hole with a horizon at R = 2µ and singularity at R = +0. Collinear case. For collinear vectors λ 1 , λ 2 from (6) obeying λ 1 + λ 2 = 0 we obtain ν i = 0, a = 2 and where λ 1 λ 2 > 0. By changing the radial variable, R = r − P, we get a little extension of the solution from Ref. [17] The metric in these variables coincides with the wellknown Reissner-Nordström metric governed by two parameters: GM > 0 and Q 2 < 2(GM) 2 . We have two horizons in this case. The electric and magnetic charges are not independent but obey Eqs. (24). Note that to be consistent with the literature the net charge here is related to the charge of the Reissner-Nordström black hole as follows Q 2 = 2Q 2 RN .

Gravitational mass and scalar charges
The definition of the ADM gravitational mass is obtained from Eq. (9) in the weak field regime by comparing with In turn, the scalar charge vector Q ϕ = (Q 1 ϕ , Q 2 ϕ ) is derived from (10) in the weak field regime using the following definition: where ν is given by Eq. (16). By combining relations (27) and (28) we obtain the following identity This formula does not contain vectors λ s . The identity (29) may be verified by using (14), (17) and the following relation For further analyses it is convenient to introduce the following dimensionless parameters We obtain The function f * (p, a) is monotonically increasing in p on (0, +∞) for any a ∈ (0, 2] since Due to (32) and lim p→+∞ f * (p, a) = 4/a 2 relation (32) defines a one-to-one correspondence between p ∈ (0, +∞) and q ∈ (0, 2 √ 2 a ) for any (fixed) a ∈ (0, 2]. Thus, we have The inverse map p(q) = p(q, a) is defined for any a ∈ (0, 2] as follows

Black hole thermodynamics
In this subsection we consider black hole thermodynamics by calculating the Hawking temperature and entropy, checking the first law (of black hole thermodynamics) and testing the Smarr relation.
To this end, for simplicity here we puth = c = k B = 1. The Bekenstein-Hawking (area) entropy S = A/(4G), associated with the black solution (12) at the horizon at R = 2µ, where A is the horizon area, reads while the related Hawking temperature is following one It may be verified that relations (27), (36) and (37) imply the first law of the black hole thermodynamics dM = T dS + ΦdQ (38) as well as the Smarr formula where Relations (38), (39) may be presented in the following form i = 1, 2. In derivation of relations (41), (42) the following identity is used Let us clarify the physical sense of potentials (43). The first relation in (11) for F (1) = dA (1) , has a special solution for 1-form: Thus, we get i.e. Φ 1 is coinciding up to a factor 1/(2G) with the value of the zero component of the first Abelian gauge field A (1) , or electric potential, (in chosen gauge) for the field of electric charge at the horizon. Now let us consider the magnetic term in (11). The calculation of Hodge-dual gives us * F (2) and hence (see (10)) For S-dual 2-form we get and we can choose a corresponding 1-form as follows Hence, i.e. Φ 2 is coinciding up to a factor 1/(2G) with the value of the zero component of the dual Abelian gauge fieldÃ (2) , or dual electric potential, (in chosen gauge) at the horizon, which corresponds to the field of magnetic charge modulated by scalar fields.

Quasinormal modes
In this section we derive quasinormal modes (in eikonal approximation) for our static and spherically symmetric solution with the metric given (initially) in the following general form where A(u), B(u), C(u) > 0 and dΩ 2 = dθ 2 + sin 2 θ dφ 2 . Note that in this section and below we use the Planck units, i.e. we puth = G = c = 1.
We consider a test massless scalar field defined in the background given by the metric (54). The equation of motion in general is written in the form of the covariant Klein-Fock-Gordon equation where µ, ν = 0, 1, 2, 3. In order to solve this equation we separate variables in function Ψ as follows where Y lm are the spherical harmonics. Equation (55), after using (56) yields the equation describing the radial function Ψ * (u) and having a Schrödinger-like form and γ ′ = dγ/du, and l is the multipole quantum number, l = 0, 1, . . . . Taking into account above expressions one can examine a dyon-like black hole solution which has the following form where f (R) and C(R) according to Eq.(10) can be written as where H(R) = 1 + P/R is the moduli function, µ, P > 0 and 0 < a ≤ 2 as shown earlier. After using the "tortoise" coordinate transformation the metric takes the following form For the choice of the tortoise coordinate as a radial one (u = R * ) we have A = B = f and Thus, the Klein-Fock-Gordon equation becomes where ω is the (cyclic) frequency of the quasinormal mode and V = V (R) = V (R(R * )) is the effective potential so that V is the eikonal part of the effective potential. Here and below we denote F ′ = dF dR * = f dF dR . In what follows we consider the so-called eikonal approximation when l ≫ 1.
The maximum of the eikonal part of the effective potential is found from the condition or, equivalently, which yields the corresponding radius The inequality (72), which is valid for 0 < a ≤ 2, is a trivial one.
It may be readily verified by using quadratic equation for Z = R − 2µ and D > 0 that for all 0 < a ≤ 2. Here R 0,− is another root of the quadratic equation (70) , which corresponds to the "location" under the horizon and is irrelevant for our consideration. The maximum of the eikonal part of the effective potential thus becomes In Fig. 1 we plot the reduced eikonal part of the effective potential V /(l(l + 1)) (l = 0) as a function of the radial coordinate R (left panel), and tortoise coordinate R * (right panel). As can be seen from examples presented in figure for special fixed values of P and µ, the maximum of the effective potential is largest for a = 0 case and smallest for a = 2 case. The case with a = 1 is in the middle. At large distances the effective potential tends to zero, as expected.
The second derivative with respect to the tortoise coordinate is given by where D is defined in (72). The square of the cyclic frequency in the eikonal approximation reads as following [12,13] where l ≫ 1 and l ≫ n. Here n = 0, 1, . . . is the overtone number. By choosing an appropriate sign for ω we get the asymptotic relations (as l → +∞) on real and imaginary parts of complex ω in the eikonal approximation where H 0 = 1 + P R 0 , F 0 = 1 − 2µ R 0 and R 0 , D are given by (71), (72), respectively.
In Fig. 2 we constructed real part of the QNM frequency, Re(ω), as a function of parameter P for different values of a and µ = 1/2. In the right panel we have a three-dimensional plot of Re(ω) versus P and a. Here one can notice that in the limiting case when a = 0 we recover constant Re(ω) identical to the case of the Schwarzschild black hole.
In Fig. 3 we constructed the imaginary part of the QNM frequency with negative sign, -Im(ω), as a function of parameter P for different values of a and µ = 1/2 in analogy to Fig. 2. At first sight Figs. 2 and 3 seem similar. However, according to Eqs. (78) and (79) this is not the case.
Remark. It was shown in Ref. [41] that parameters of the unstable circular null geodesics around stationary spherically symmetric and asymptotically flat black holes are in correspondence with the eikonal part of quasinormal modes of these black holes. See also [42,43] and references therein. But as it was pointed out in Ref. [44] this correspondence is valid if: (a) perturbations are described by a "good" effective potential, ( b) "one is limited by perturbations of test fields only, and not of the gravitational field itself or other fields, which are non-minimally coupled to gravity." Here we do not consider this correspondence for our solution, postponing this to future publication.

Limiting cases corresponding to the Schwarzschild and Reissner-Nordström black holes
In this section we consider two limiting cases a = +0 and a = 2 corresponding to the Schwarzschild and Reissner-Nordström metrics, respectively. a) Let us first consider the case when a = +0. This limit may be obtained in a strong coupling regime when where e 1 2 = e 1 2 = 1, and In this case the relations (78) and (79) for QNM in the eikonal approximation read as follows where r 0 = R 0 = 3M corresponds the position where the black-hole effective potential attains its maximum. Note that r 0 = 3M is the radius of the photon sphere for the Schwarzschild black-hole. These results have been obtained in Ref. [7] and our outcomes are consistent with them. b) Now let us consider the case when a = 2. As was mentioned above this takes place for collinear vectors λ 1 , λ 2 . One can also obtain the limit a = 2 in the weak coupling regime when dilatonic coupling vectors obey (80) and In this case the eikonal QNM (see (78) and (79)) read where r 0 = 3M/2+(1/2) 9M 2 − 4Q 2 = R 0 +P corresponds to the position of the unstable, circular photon orbit in the Reissner-Nordström spacetime. These results have been obtained in Ref. [45] (for n = 0) and our outcomes are compatible with them when the relation (for our notation) Q 2 = 2Q 2 RN is applied.

Hod conjecture
Here we test/check the conjecture formulated by Hod [40] on the existence of quasi-normal modes obeying the inequality where T H is the Hawking temperature.
Recently the Hod conjecture has been tested in theories with higher curvature corrections such as the Einstein-Dilaton-Gauss-Bonnet and Einstein-Weyl for the Dirac field [46]. It has been shown that in both theories the Dirac field obeys the Hod conjecture for the whole range of black-hole parameters [46].
Here we test/check this conjecture by using eikonal relations (79) for Im(ω) and the relation for the Hawking temperature (37). For our purpose it is sufficient to check the validity of the inequality for all p = P/µ > 0, where In (88) we use the limiting "eikonal value" given by the first term in (79) for the lowest overtone number n = 0.
In Table 1 we present the results for the numerical testing of the Hod bound by using obtained relations for the eikonal QNM in the ground state n=0. It turned out that the Hod bound is valid (in the eikonal regime) in the range 0 < a ≤ 1. There are maximum y max = y max (a) and limiting y lim = y lim (a) values of function y(p, a) for different values of parameter a in the considered range. It may be verified that for 0 < a < 1 and y lim (1) = 0. The relation for y lim (a) just follows from for 0 < a < 1.
We denote the value of p corresponding to y max (a) as p 0 = p 0 (a). For increasing a, the values of p 0 (a) and y max (a) increase and y lim (a) decrease. We obtain y max (1) ≈ 0.847 and y lim (+0) = 0. For decreasing a, both y max (a) and y lim (a) approach a finite value, corresponding to the Schwarzschild case 4 3 √ 3 ≈ 0.7698 when a → 0. In Fig. 4 we illustrate y = y(p, a) as a function of p. In the left panel we build two dimensional plot for a = 0.2, 0.4, 0.6, 0.8, 1.0 and in the right panel we construct three dimensional plot for the range 0 < a ≤ 1, where the Hod conjecture holds. Thus, we are led to the following proposition.
Proposition. The dimensionless parameter y = y(p, a) from (88) obeys the inequality: y(p, a) < 1 for all p > 0 and a ∈ (0, 1]. For 0 < a < 1 this proposition is proved analytically in Appendix. For a = 1 it is justified by our numerical bound y < y max (1) ≈ 0.847.
Here the limit p = +∞ corresponds to extremal (black hole) case which is not considered here.
Remark. Recently, in Ref. [47] some example of the violation of the Hod conjecture has been found for certain (scalar gravitational) perturbations around D = 5 Gauss-Bonnet-de Sitter black hole solution.
In Table 2 we present some critical values p crit , which are obtained through the condition y(p crit ) = 1 (with y calculated for the ground state n=0) and q crit corresponding to p crit according to Eq. (94) for various values of the model parameter a obeying 1 < a ≤ 2.
Here we use the following relation (see Eq. (32)) where q ext corresponds to extremal case. (Here G = 1.) In Fig. 5 we illustrate y = y(p, a) as a function of p. In the left panel we build two dimensional plot for a = 1.2, 1.3, 1.4, 1.6, 2.0 and in the right panel we construct three dimensional plot for the range 1 < a ≤ 2. In this case the Hod inequality (88) holds in the range p ∈ (0, p crit (a)), while for p ∈ (p crit (a), +∞) it breaks. Remark. In Ref. [48], the eikonal QNM frequencies for charged scalar field in the space-time of a charged Reissner-Nordström black hole were obtained analytically in the regime l 2 ≥ Qq * ≥ l, where Q is the electric charge of the black hole and q * is the electric charge of the field. In this regime the obtained fundamental frequencies were shown to saturate the Hod bound. It should be noted that this result can not be applied to our analysis for a = 2, since we deal here with q * = 0 case.

Conclusions
We have examined a non-extremal black hole dyon-like solution in a 4-dimensional gravitational model with two scalar fields and two Abelian vector fields proposed in Ref.
[30]. The model contains two vectors of dilatonic coupling vectors λ s = 0, s = 1, 2, obeying λ 1 = − λ 2 and additional relations (18). We have also presented some physical parameters of the solutions: gravitational mass M, scalar charges Q i ϕ , Hawking temperature, black hole area entropy. In addition, we considered the first law of black hole thermodynamics and checked the validity of the Smarr relation for our model.
In fact this is a special solution with dependent electric and magnetic charges, see (17). In the case of non-collinear vectors λ 1 , λ 2 the metric of the solution describes a black hole with one (external horizon) and singularity hidden by it. For collinear vectors λ 1 , λ 2 the metric coincides with the Reissner-Nordström metric possessing two horizons and hidden singularity.
We have studied the solutions to massless (covariant) Klein-Fock-Gordon equation in the background of our static and spherically symmetric metric, by using the variable separation method. The Klein-Fock-Gordon equation is simplified in the tortoise coordinate leading to radial equation gov-erned by effective potential. This potential contains the parameters of solution such as P > 0, µ > 0 and dimensionless parameter a ∈ (0, 2] depending upon the coupling vectors λ s which are the initial parameters of the model. The physical quantities, such as mass, color charges and scalar charges contain some of these parameters. Here we mainly focused on the eikonal part of the effective potential and calculated the value of the radial coordinate (radius) R 0 corresponding to the maximum of this part of the effective potential. Knowing the maximum of the eikonal part of the effective potential and corresponding radius, we have calculated the cyclic frequencies of the quasinormal modes in the eikonal approximation. We have also considered two limiting cases reducing to the Schwarzschild and Reissner-Nordström solutions, when the parameter of the solution a accepts two distinct values, i.e. a = +0 and a = 2, respectively. Thus, we have made sure that our outcomes are consistent with the previous results in the literature.
We have also tested the validity of the Hod conjecture for our solution by using QNM frequences in the eikonal approximation with the lowest value of the overtone number n = 0. It turned out that the Hod assumption holds in the range of 0 < a ≤ 1. The conjecture is valid in this range since it is supported by examples of states with large enough values of angular number l. For 1 < a ≤ 2 we have found that the Hod bound is satisfied for n = 0, and small enough values of charge Q (Q/M < q crit (a)) and big enough values of l (l ≫ 1).
It would be interesting to explore in detail QNM frequencies in the vicinity of a = 0 and a = 2, by using the treatment of Ref. [49], e.g. extending the results for the Schwarzschild and Reissner-Nordström solutions by using expansion in a small parameter (a or a − 2). Another issue of interest is the numerical calculation of QNM frequencies by using higher-order WKB formula for certain lower levels (labelled by l and n), see Ref. [50], e.g. verifying the Hod conjecture for 1 < a < 2, calculating grey-body factors etc. All these issues may be addressed in our future studies.