By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. ...By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. It is shown that the coupling between the scalar field and background metric affects the quasinormal frequencies. At low overtones, both the real part and the magnitude of imaginary part increase with the couple factor ξ. For the larger ξ, both of them are almost linearly related to the couple factor. At high overtones, it is found that the frequency formula of the quasinormal modes is 2πω/κ = ln （ 1 ＋ 2 cos√9-24ξ/5 π） - i（2n ＋ 1）π, which means that 5 when ξ is larger, the real part is the linear function of ξ^1/2.展开更多
基金Supported by the FANEDD under Grant No 2003052, the Natural Science Foundation of Hunan Province of China under Grant No 05JJ40012 and the Hunan Normal University Natural Science Foundation under Grant No 22040639.
文摘By using the third-order Wentzel-Kramers-Brillouin approximation and the monodromy methods, the quasnormal modes of a coupled scalar field in the canonical non-rotating acoustic black hole spacetime are investigated. It is shown that the coupling between the scalar field and background metric affects the quasinormal frequencies. At low overtones, both the real part and the magnitude of imaginary part increase with the couple factor ξ. For the larger ξ, both of them are almost linearly related to the couple factor. At high overtones, it is found that the frequency formula of the quasinormal modes is 2πω/κ = ln （ 1 ＋ 2 cos√9-24ξ/5 π） - i（2n ＋ 1）π, which means that 5 when ξ is larger, the real part is the linear function of ξ^1/2.
