2005/11/30 by D. K. Park, D.K. Park
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #hep-th
paper · pdf · doi:10.1016/j.physletb.2005.12.048
published as Phys.Lett.B633:613-617,2006 · 15 pages, 1 eps figure: V2 one more reference added. The derivtaion of the effective potential is explained in detail. Version of PLB
arxiv created 2005/12/22 · openalex publication_date 2005/12/30 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
The asymptotic quasinormal frequencies of the brane-localized (4+n)-dimensional black hole are computed. Since the induced metric on the brane is not an exact vacuum solution of the Einstein equation defined on the brane, the real parts of the quasinormal frequencies ω do not approach to the well-known value TH ln 3 but approach to TH ln kn, where kn is a number dependent on the extra dimensions. For the scalar perturbation Re(ω/ TH) = ln 3 is reproduced when n = 0. For n ≠ 0, however, Re(ω/ TH) is smaller than ln 3. It is shown also that when n > 4, Im(ω/ TH) vanishes in the scalar perturbation. For the gravitational perturbation it is shown that Re(ω/ TH) = ln 3 is reproduced when n = 0 and n = 4. For different n, however, Re(ω/ TH) is smaller than ln 3. When n = ∞, for example, Re(ω/ TH) approaches to ln (1 + 2 cos √(5) π) ≈ 0.906. Unlike the scalar perturbation Im(ω/ TH) does not vanish regradless of the number of extra dimensions.