TY - JOUR

T1 - Scalar-gravitational perturbations and quasinormal modes in the five dimensional Schwarzschild black hole

AU - Cardoso, Vitor

AU - Lemos, José P.S.

AU - Yoshida, Shijun

N1 - Copyright:
Copyright 2020 Elsevier B.V., All rights reserved.

PY - 2003/12/1

Y1 - 2003/12/1

N2 - We calculate the quasinormal modes (QNMs) for gravitational perturbations of the Schwarzschild black hole in the five dimensional (5D) spacetime with a continued fraction method. For all the types of perturbations (scalar-gravitational, vector-gravitational, and tensor-gravitational perturbations), the QNMs associated with l = 2, l = 3, and l = 4 are calculated. Our numerical results are summarized as follows: (i) The three types of gravitational perturbations associated with the same angular quantum number l have a different set of the quasinormal (QN) frequencies; (ii) There is no purely imaginary frequency mode; (iii) The three types of gravitational perturbations have the same asymptotic behavior of the QNMs in the limit of the large imaginary frequencies, which are given by ωTH -1 → log 3 + 2πi(n + 1/2) as n → ∞, where ω, TH, and n are the oscillation frequency, the Hawking temperature of the black hole, and the mode number, respectively.

AB - We calculate the quasinormal modes (QNMs) for gravitational perturbations of the Schwarzschild black hole in the five dimensional (5D) spacetime with a continued fraction method. For all the types of perturbations (scalar-gravitational, vector-gravitational, and tensor-gravitational perturbations), the QNMs associated with l = 2, l = 3, and l = 4 are calculated. Our numerical results are summarized as follows: (i) The three types of gravitational perturbations associated with the same angular quantum number l have a different set of the quasinormal (QN) frequencies; (ii) There is no purely imaginary frequency mode; (iii) The three types of gravitational perturbations have the same asymptotic behavior of the QNMs in the limit of the large imaginary frequencies, which are given by ωTH -1 → log 3 + 2πi(n + 1/2) as n → ∞, where ω, TH, and n are the oscillation frequency, the Hawking temperature of the black hole, and the mode number, respectively.

KW - Black Holes

KW - Classical Theories of Gravity

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U2 - 10.1088/1126-6708/2003/12/041

DO - 10.1088/1126-6708/2003/12/041

M3 - Article

AN - SCOPUS:23044451382

VL - 7

SP - 957

EP - 970

JO - Journal of High Energy Physics

JF - Journal of High Energy Physics

SN - 1126-6708

IS - 12

ER -