Research Article Resonance Spectra of Caged Stringy Black Hole and Its Spectroscopy I. Sakalli and G. Tokgoz Department of Physics, Eastern Mediterranean University, Gazimagosa, Northern Cyprus, Mersin 10, Turkey Correspondence should be addressed to I. Sakalli; izzet.sakalli@emu.edu.tr Received 7 November 2014; Revised 20 January 2015; Accepted 20 January 2015 Academic Editor: George Siopsis Copyright © 2015 I. Sakalli and G. Tokgoz. Tis 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. Te publication of this article was funded by SCOAP 3 . Maggiore’s method (MM), which evaluates the transition frequency that appears in the adiabatic invariant from the highly damped quasinormal mode (QNM) frequencies, is used to investigate the entropy/area spectra of the Garfnkle–Horowitz–Strominger black hole (GHSBH). Instead of the ordinary QNMs, we compute the boxed QNMs (BQNMs) that are the characteristic resonance spectra of the confned scalar felds in the GHSBH geometry. For this purpose, we assume that the GHSBH has a confning cavity (mirror) placed in the vicinity of the event horizon. We then show how the complex resonant frequencies of the caged GHSBH are computed using the Bessel diferential equation that arises when the scalar perturbations around the event horizon are considered. Although the entropy/area is characterized by the GHSBH parameters, their quantization is shown to be independent of those parameters. However, both spectra are equally spaced. 1. Introduction Currently, one of the greatest projects in theoretical physics is to unify general relativity (GR) with quantum mechanics (QM). Such a new unifed theory is known as the quantum gravity theory (QGT) [1]. Recent developments in physics show that our universe has a more complex structure than that predicted by the standard model [2]. Te QGT is considered to be an important tool that can tackle this problem. However, current QGT still requires further exten- sive development to reach completion. Te development of the QGT began in the seventies when Hawking [3, 4] and Bekenstein [5–9] considered the black hole (BH) as a quantum mechanical system rather than a classical one. In particular, Bekenstein showed that the area of the BH should have a discrete and equally spaced spectrum A  =ℎ=8ℎ, (=0,1,2,...), (1) where  is the undetermined dimensionless constant and  is of the order of unity. Te above expression also shows that the minimum increase in the horizon area is ΔA min = ℎ. Bekenstein [7, 8] also conjectured that for the Schwarzschild BH (also for the Kerr-Newman BH) the value of  is 8 (or =1). Following the seminal work of Bekenstein, various methods have been suggested to compute the area spectrum of the BHs. Some methods used for obtaining the spectrum can admit that the value of  is diferent than that obtained by Bekenstein; this has led to the discussion of this subject in the literature (for a review of this topic, see [10] and references therein). Among those methods, the MM’s results [11] show a perfect agreement with Bekenstein’s result by modifying the Kunstatter’s [12] formula as  adb =∫  Δ , (2) where  adb denotes the adiabatic invariant quantity and Δ=  −1 −  represents the transition frequency between the subsequent levels of an uncharged and static BH with the total energy (or mass) . However, the researchers [13–15] working on this issue later realized that the above defnition is not suitable for the charged rotating (hairy) BHs that the generalized form of the defnition should be given by  adb =∫  Δ , (3) Hindawi Publishing Corporation Advances in High Energy Physics Volume 2015, Article ID 739153, 7 pages http://dx.doi.org/10.1155/2015/739153