Spacing of the entropy spectrum for KS Black hole in Horava-Lifshitz gravity

Abstract

In this paper we present the spectrum of entropy/area for Kehagias-Sfetsos (KS) black hole in Ho$\check{\text{r}}$ava-Lifshitz (HL)gravity via quasi-normal modes (QNM) approach. We show that in the massive case the mass parameter $\mu$ disappears in the entropy spectrum and only the quasinormal modes modified by a term which is proportional to the mass square term. Our calculations show that the charge like parameter $\frac{1}{2\omega }=Q^2$ appears in the surface gravity and our calculations can be applied to any spherically symmetric spacetime which has only one physically acceptable horizon. Our main difference between our calculations and what was done in \cite{1} is that the portion of charge and mass is included explicitly in the surface gravity and consequently in the QNM expression. Since the imaginary part of the QNM is related to the adiabatic invariance of the system and also to the entropy, surprisingly the mass parameter do not appear in the entropy spectrum. Our conclusion supported by some acclaims about that the scalar field parameters (charges) can not change the fundamental parameters in the 4-dimensional black holes.

arXiv comment9 pages, no figure

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• Self-gravitational Interaction in z = 4 Horava-Lifshitz Gravity
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• Spectroscopy of Stringy Black Hole
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