Advances in High Energy Physics

Volume 2018, Article ID 3270790, 7 pages

https://doi.org/10.1155/2018/3270790

## Spectroscopy of Lifshitz Black Hole

Physics Department, Eastern Mediterranean University, Famagusta, Northern Cyprus, Mersin 10, Turkey

Correspondence should be addressed to Gulnihal Tokgoz; rt.ude.ume@zogkot.lahinlug

Received 22 May 2018; Accepted 8 July 2018; Published 17 July 2018

Academic Editor: Farook Rahaman

Copyright © 2018 Gulnihal Tokgoz and Izzet Sakalli. 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

We studied the thermodynamics and spectroscopy of a -dimensional, Lifshitz black hole (LBH). Using Wald’s entropy formula and the Hawking temperature, we derived the quasi-local mass of the LBH. Based on the exact solution to the near-horizon Schrödinger-like equation (SLE) of the massive scalar waves, we computed the quasi-normal modes of the LBH via employing the adiabatic invariant quantity for the LBH. This study shows that the entropy and area spectra of the LBH are equally spaced.

#### 1. Introduction

Ever since the publication of the seminal papers of Bekenstein and Hawking [1–3], it has been known that black hole (BH) entropy () should be quantized in discrete levels as discussed in detail by Bekenstein [4–7]. The proportionality between and BH area () is justified from the adiabatic invariance [8] properties of area, that is, . Therefore, should also be quantized in equidistant levels to account for the discrete . Bekenstein [5, 6] proposed that, for the family of Schwarzschild BHs, should have the following discrete, equidistant spectrum:where is known as the undetermined dimensionless constant. According to (1), the minimum increase in the horizon area becomes for the Schwarzschild BH () [9–11]. Following the seminal works of Bekenstein, new methods have been developed to derive the entropy/area spectra of the numerous BHs (see [12] and references therein). Among them, Maggiore’s method (MM) [9] fully supports Bekenstein’s result (1). In fact, MM [9] was based on Kunstatter’s study [13], in which the adiabatic invariant quantity () is expressed as follows:

where denotes the transition frequency between the successive levels of a BH having mass . Further, (2) was generalized to the hairy BHs (massive, charged, and rotating ones) as follows (see [14] and references therein):

where is the temperature of the BH. Bohr-Sommerfeld quantization rule [15] states that acts as a quantized quantity when the highly excited modes () are considered. In such a case, the imaginary part of the frequency dominates the real part of the frequency (), implying that . Meanwhile, for the first time, Hod [16, 17] argued that the quasi-normal modes (QNMs) [18, 19] can be used for computing transition frequency. Hod’s arguments inspired Maggiore who considered the Schwarzschild BH as a highly damped harmonic oscillator (i.e., ) and managed to rederive Bekenstein’s original result (1) using a different method. Today, there are numerous studies in the literature in which MM has been employed for various BHs (see, e.g., [20–25]).

This study mainly explores the entropy/area spectra of a four-dimensional Lifshitz BH [26] possessing a particular dynamical exponent . To analyze the physical features of the Lifshitz BH (LBH) geometry, we first calculate its quasi-local mass [27] and temperature via Wald’s entropy [28] and statistical Hawking temperature formula [29, 30], respectively. QNM calculations of the LBH must be performed in order to implement the MM successfully. To this end, we consider the Klein-Gordon equation (KGE) for a massless scalar field in the LBH background. Separation of the angular and the radial equations yields a Schrödinger-like wave equation (SLE) [31]. Asymptotic limits of the potential (36) show that the effective potential may diverge beyond the BH horizon for the massive scalar particle; thus, in the far region, the QNMs might not be perceived by the observer. Hence, following a particular method [23, 32–35], we focus our analysis on the near-horizon (NH) region and impose the boundary conditions (45): ingoing waves at the event horizon and no wave at spatial infinity (since at infinity the effective potential of Schrödinger-like wave equation is divergent). After getting NH form of the SLE, we show that the radial equation is reduced to a confluent hypergeometric (CH) differential equation [36]. Performing some manipulations on the NH solution and using the pole structure of the Gamma functions [36], we show how one finds out the QNMs as in [32, 33, 37–40]. The imaginary part of the QNMs is used in (3), and the quantum spectra of entropy and area of the LBH are obtained.

The following statements elaborate on the organization of this study. In Section 2, we briefly introduce the LBH metric. In addition, we present the derivation of of the LBH based on Wald’s entropy formula. Section 3 is devoted to the separation of the KGE and finding the effective potential . Next, we solve the NH SLE and show how QNMs are calculated. Then, we compute the entropy/area spectra of the LBH. Finally, we draw our conclusions in Section 4 (throughout this work, the geometrized unit system is used: and ).

#### 2. LBH Spacetime

In this section, we introduce the four-dimensional Lifshitz spacetime and its special case, that is, LBH [26]. Conformal gravity (CG) covers gravity theories that are invariant under Weyl transformations. CG, which is adapted to static and asymptotically Lifshitz BH solutions, has received intensive attention from the researchers studying condensed matter and quantum field theories [41]. The Lifshitz BHs are invariant under anisotropic scale and characterize the gravitational dual of strange metals [42].

The action of the Einstein-Weyl gravity [26] is given by

where , , and (constant), which diverges ( with and/or . The Lifshitz BH solutions exist in the CG theory for both and [26, 43]; however, when and , Lifshitz BHs appear in the Horava–Lifshitz gravity [26, 44, 45].

Now, we focus on the LBH of the CG theory whose metric is given by [26]:

where the metric function is defined by

In the above metric, which is conformal to (A)dS (AdS if and dS if ) [26], , , and stand for 2-torus (), unit 2-sphere (), and unit hyperbolic plane (), respectively [45]. The metric solution has a curvature singularity at , which becomes naked for . There is an event horizon for solution expressed as follows [26, 45]:

Note that the requirement of is conditional on this inequality: . When , the solution becomes extremal. Throughout this study, for simplicity, we consider the choice of for which the solution corresponds to a dS BH. Thus, the metric function becomes

Thus, at spatial infinity, the Ricci and Kretschmann scalars of the LBH can be found as follows:

By performing the surface gravity calculation [1, 2, 30], we obtain

Therefore, the Hawking or BH temperature [30] of the LBH reads

##### 2.1. Mass Computation of Z0LBH via Wald’s Entropy Formula

The GR unifies space, time, and gravitation and the gravitational force is represented by the curvature of the spacetime. Energy conservation is a sine qua non in GR as well. Because the metric (5) of LBH represents a non-asymptotically-flat geometry, one should consider the quasi-local mass [27], which measures the density of matter/energy of the spacetime. In this section, we shall employ Wald’s entropy calculation [29, 30] and derive using Wald’s entropy formula. To this end, we follow the study of Eune and Kim [28].

Starting with the time-like Killing vector , which describes the symmetry of time translation in a spacetime, Wald’s entropy is expressed by [29, 30] as

where

Here, and are the surface gravity and the induced metric on a hypersurface of the horizon (here 2-sphere with ), respectively. is the four-vector velocity defined as the proper velocity of a fiducial observer moving along the orbit of (where is a normalization constant), which must satisfy at spatial infinity. Thus, one can immediately see that . is called the Noether potential [46, 47], which is given by

with

The surface gravity can be calculated by [30]

To have an outward unit vector on , the equality must also be satisfied. Hence, one can get

On the contrary, is the four-vector velocity and is given by

with

Therefore, the nonzero components of are found to be

In sequel, the four-vector velocity reads

The nonzero components of (15) are obtained as follows:

One can verify that . The latter result yields that the second term of the Noether potential vanishes. Therefore, we have

The nonzero components of are as follows:

After substituting those findings into (14), we find the nonzero components of the Noether potential:

Thus, from (20) and (25), is found as

and, in sequel computing the entropy through the integral formulation (12), we obtain

The above result is fully consistent with the Bekenstein-Hawking entropy. The quasi-local mass can be derived from this entropy by integrating the first law of thermodynamics . After some manipulation, one easily finds the following result:

which matches with the quasi-local mass computation of Brown and York [27].

#### 3. QNMs and Spectroscopy of LBH

In this section, we shall study the QNMs and the entropy of a perturbed LBH via MM [9]. QNMs of a considered BH can be derived by solving the eigenvalue problem of the KGE with the proper boundary conditions. The boundary condition at the horizon implies that there are no outgoing waves at the event horizon (i.e., only ingoing waves carry the QNMs at the event horizon) and the boundary condition at spatial infinity imposes that only outgoing waves are allowed to survive at spatial infinity. The second boundary condition is appropriate for bumpy shape effective potential that dies off at the two ends. Yet, as seen in (36) and shown in Figure 1, the potential never terminates at spatial infinity; instead it diverges for very massive () scalar particles. Thus, the potential blocks the waves that come off from the BH and prevents them from reaching spatial infinity. Hence, in this section, we will consider the very massive scalar particles and employ the particular method of [23, 32–35], in which only the QNMs are defined to be those for which one has purely ingoing plane wave at the horizon and no wave at spatial infinity (see (44). Namely, we will find the QNMs of the LBH using their NH boundary condition. For this purpose, we first consider the massive KGE: