Advances in High Energy Physics

Volume 2017, Article ID 9891231, 10 pages

https://doi.org/10.1155/2017/9891231

## On Quasinormal Modes for Scalar Perturbations of Static Spherically Symmetric Black Holes in Nash Embedding Framework

^{1}Instituto de Física, Universidade de Brasília, 70910-900 Brasília, DF, Brazil^{2}Faculdade Gama, Universidade de Brasília, Setor Leste (Gama), 72444-240 Brasília, DF, Brazil^{3}Casimiro Montenegro Filho Astronomy Center, Itaipu Technological Park, Federal University of Latin-American Integration, P.O. Box 2123, 85867-970 Foz do Iguaçu, PR, Brazil

Correspondence should be addressed to Sergio C. Ulhoa; moc.liamg@aohlu.cs

Received 15 October 2016; Revised 21 December 2016; Accepted 15 January 2017; Published 14 February 2017

Academic Editor: Torsten Asselmeyer-Maluga

Copyright © 2017 Sergio C. Ulhoa et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.

#### Abstract

In this paper we investigate scalar perturbations of black holes embedded in a five-dimensional bulk space. The quasinormal frequencies of such black holes are calculated using the third order of Wentzel, Kramers, and Brillouin (WKB) approximation for scalar perturbations. The high overtones of quasinormal modes indicate a resonant-like set of black holes suggesting a serious constraint of embedding models in five dimensions.

#### 1. Introduction

The black hole solutions can be perturbed by some matter field; then it leads to oscillations, which can be explained by an analogy with a vibrating string; in such a system the oscillations decrease with time as the string loses energy to the environment [1]. Similarly to the string, where its frequency can be expressed by a complex parameter called quasinormal frequency, the perturbations of black holes evolve with time as an oscillation with complex frequency, in which the real part is responsible for the period of oscillation and the imaginary part is responsible for damping or amplification. Thus proper oscillations of black holes are also called quasinormal modes.

Historically, the theoretical study on perturbations of black holes began with the seminal paper of Regge and Wheeler in 1957 in which they studied the stability of Schwarzschild black hole submitted to small perturbations [2]. In the 70s, the quasinormal modes were used by Vishveshwara in calculations of scattering of gravitational waves by a Schwarzschild black hole [3]. Since then, the study of this issue was directed to several problems. Black holes stability is an example of this importance. The relevance of studying the stability of these astrophysical objects is the possibility of understanding theories in higher dimensions as aspects of brane-world and string theory [4, 5] and variants. Since the uniqueness theorem is not applicable to more than four dimensions, stability can be the criterion to select physical solutions [6, 7]. Another important application of the quasinormal modes of black holes is in the study of the ADS/CFT correspondence [8], whereby the imaginary part of the quasinormal fundamental frequency describes the thermalization time in a conformal invariant field theory in the border of the anti-de-Sitter space-time. In addition, there are prospects that in the near future more oscillations of astrophysical black holes can be observed using gravitational waves detectors as in LIGO Scientific Collaboration and Virgo Collaboration [9] and be an important tool to constrain higher dimensional models [10, 11]. This fact is relevant in the sense that quasinormal modes carry information about stellar objects, such as mass, charge, and angular momentum.

Considering the relevance of the quasinormal modes, in this work we study scalar perturbation of a black hole embedded in a five-dimensional bulk space by calculating its quasinormal frequencies. In this sense, this paper is organized as follows. In Section 2, we present a summary of the Nash embedding theorem to study the induced four-dimensional equations embedded in a five-dimensional bulk space. In Section 3, we present the induced potential in embedded spherically symmetric vacuum solution. In Section 4, we discuss scalar perturbations. In Section 5, we present the quasinormal modes for treated system using WKB approach and the resulting effective potential. In Section 6, we present our concluding remarks.

#### 2. Embedded Induced Four-Dimensional Equations

The proof of the Poincaré conjecture by Perelman [12, 13] suggests a new paradigm for geometry and in particular for Einstein’s gravitation and cosmology, namely, the possibility that we can deform space-time in arbitrary directions, changing its shape. It has its origins from a solution for the Riemann curvature ambiguity was conjectured by L. Schlaefli in 1871, proposing that the Riemann manifolds should be embedded in a larger bulk space, such that its Riemann curvature would act as a curvature reference for all embedded manifolds, just like the flat Euclidean space which acts as a curvature reference for surfaces. The Schlaefli conjecture is the origin of the embedding problem for Riemann’s geometry. Formally we may write his proposal asTo detail this, we must rewrite this expression in terms of components in a suitable reference frame. This can be done in an arbitrary vielbein defined in the bulk and then by separating the bulk curvature tensor in normal and tangent components. With the purpose of understanding the meaning of the Schlaefli proposal we write these components in the Gaussian frame defined by the embedding map itself. In this frame the components of the extrinsic terms appear as the extrinsic curvature component. This allows us to relate different geometries with different properties through a differential embedding.

In order to make an appropriate embedding between smooth (differentiable) geometries, we use the Nash embedding theorem [14] in order to propose a new theoretical structure able to relate it to a physical theory. Nash showed that any embedded perturbed metric can be generated by a continuous sequence of small metric perturbations of a given initially unperturbed geometry by means ofor, equivalently,where is the coordinate related to extra dimensions. Since Nash’s smooth deformations are applied to the embedding process, the coordinate usually noticed in rigid embedded models [15, 16] can be omitted in the process for perturbing the element line. This seems particularly interesting to astrophysical and cosmological problems in which traditionally the gravitational perturbation mechanisms are essentially plagued by coordinate gauges due to the group of diffeomorphisms.

The Einstein-Hilbert principle leads to -dimensional Einstein’s equations for the bulk metric in arbitrary coordinates where we have dispensed the bulk cosmological constant and denotes the energy-momentum tensor of the known matter and gauge fields. The constant determines the -dimensional energy scale. For the present application, capital Latin indices run from 1 to 5. Small case Latin indices refer to the only one extra dimension considered. All Greek indices refer to the embedded space-time counting from 1 to 4.

Concerning the confinement, the four-dimensionality of the space-time is an experimentally established fact associated with the Poincaré invariance of Maxwell’s equations and their dualities, also valid for Yang-Mills gauge fields restricted to four dimensions [17, 18]. Even though the duality properties can be mathematically extended to higher dimensions, we adopt it as a condition based on experimental backgrounds [19]. Therefore, all matter, which interacts with these gauge fields, must for consistency be also defined in the four-dimensional space-time. This consideration complements a physical interpretation for the Nash theorem that provides an interesting mechanism for perturbing and creating new geometries. In this five-dimensional framework present here, only the components that access higher dimensions are related to the extrinsic curvature , while the metric components are confined to the geometry as shown in (2). On the other hand, in spite of all efforts made so far, the gravitational interaction has failed to fit into a similar gauge scheme, so that the gravitational field does not necessarily have the same four-dimensional limitations, regardless of the location of its sources.

In order to recover Einstein’s gravity by reversing the embedding, the confinement of ordinary matter and gauge fields implies that the tangent components of in the above equations must coincide with where is the energy-momentum tensor of the confined sources. As it may have been already noted, we are essentially reproducing a framework similar to brane-world program [20], with the difference that we apply a dynamical differential embedding and have nothing to do with branes as those defined in string/M theory. Using the Nash embedding theorem together with the four-dimensionality of gauge fields, one can obtain the Einstein-Hilbert principle for the bulk and a -dimensional energy scale .

In addition, one can define a five-dimensional local embedding with an embedding map . We admit that the function is a regular and differentiable map with , which stands for the four embedded space-time types, and which refers to the bulk itself. The components associate with each point of a point in with coordinates . These coordinates are the components of the tangent vectors of . Accordingly, calculating the components of (4), one can find the induces equations for the embedded geometry:where now is the energy-momentum tensor of the confined matter. The quantities with and are the mean curvature and Gaussian curvature, respectively. Moreover, one definesThis tensor is independently conserved, as it can be directly verified that (semicolon denoting covariant derivative with respect to )A detailed derivation of these equations can be found in [21–23] and references therein as well as the higher dimensional case. Hereafter, we use a system of unit such that .

#### 3. Induced Potential in a Spherically Symmetric Vacuum Solution

As shown in a previous work [24], we start with the general static spherically symmetric induced metric that can be described by the line element aswhere we denote the functions and . Thus, one can obtain the following components for the Ricci tensor: where we have and .

From (5), the gravitational-tensor vacuum equations (with ) can be written in alternative form as where we use the contraction .

The general solution of Codazzi equations (see (6)) is given by Taking the former equation and the definition of , one can write where Consequently, we can write in terms of as

A straightforward consequence of the homogeneity of Codazzi equations (see (6)) embedded in five dimensions is that the individual arbitrariness of the functions can be reduced to a unique arbitrary function that depends on the radial coordinate. Hence, (12) turns to be with . With a straightforward calculation, one can obtain the coefficients of the metric as where is a constant. In order to constrain this arbitrariness, we look at the characteristics of the extrinsic curvature itself in the asymptotic limit, which matches the requirement to local astrophysical applications. The extrinsic curvature at infinity goes to a flat space obeying the asymptotically conformal flat condition. This can be understood as the following form:Since the function must be analytical at infinity, one can write the simplest optionwhere the sum is upon all scalar potentials and the indices and are real numbers. Since these scalar potentials have their origin in the extrinsic curvature they do not remain confined in the embedded geometry propagating in the extra dimension. The index represents all the set of scalar fields that fall off with -coordinate following the th-power law decaying. Equation (20) is essentially the representation of the effect of extrinsic curvature leading to a local modification of the space-time without producing umbilical point as expected for a spherical geometry. Depending on the variation of the function one can have a bent or stretched geometry without ripping off the manifold, and, curiously, in the same notion as pointed by Riemann himself [25]. It was shown that the parameter has cosmological magnitude [24, 26]; that is, it does not depend on individual astrophysical properties and has the same units as the Hubble constant. Its modulus is of the order of 0.677 km·s^{−1}·Mpc^{−1}. In addition, to keep the right dimension of (20) we have introduced a unitary parameter that has the inverse unit of Hubble constant and also establishes the cosmological horizon in (9). Hence, the horizons of (9) can be found when we set , and one can obtain which is a polynomial equation of order that gives a class of horizons to be defined for all allowed values of .

Using (17) and (20), one can obtain an explicit form of the coefficient given byIn terms of the correspondence principle with Einstein equations, we set , which remains valid even in the limit when in order to obtain the asymptotically flat solution. It is worth mentioning a qualitative aspect that the diffeomorphic transformations commonly known in the realm of general relativity do not necessarily apply even when . This comes from the fact that structure of the embedded space (and its relation to the bulk) breaks down the equivalence principle of general relativity. In other words, the diffeomorphism must be imposed as an assumption to recover full general relativity.

#### 4. Scalar Perturbations

In this section, we focus our attention on the study of (22) under scalar perturbations. The study of quasinormal modes can be treated by scalar fields and appropriate metrics. In this section, we construct the Klein-Gordon equation in a curved space-time embedded in a five-dimensional space-time. In order to achieve such a goal, we consider the line element in the form It is well known that the massless Klein-Gordon equation is given by or, equivalently, where . Using (23), we can write Moreover, (25) can be written as Taking the ansatz we obtainwhere are the spherical harmonics. Taking the following coordinates change , we obtain the master wave equation where we denote

If we consider (22), then we finally get

Once the potential is well defined, we plot its behaviour for different values of and , which are given in Figures 1 and 2.