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Chinese Physics C > 2025, Vol. 49 > Issue(9): 095104 DOI: 10.1088/1674-1137/add10d

Quasinormal modes of accelerating spacetime

  • School of Physics and Optoelectronics, South China University of Technology, Guangzhou 510641, China

  • We calculate the exact values of the quasinormal frequencies for massless perturbations with spin $ s\leq2 $ propagating in purely accelerating spacetime. Using two different methods, we transfer the perturbation equations into hypergeometric differential equations and obtain identical quasinormal frequencies. These purely imaginary spectra are shown to be independent of the spin of the perturbation and match those of the acceleration modes identified in accelerating black holes in the Minkowski limit. This implies that the acceleration modes originate from the purely accelerating spacetime and that the presence of black holes would deform the spectra. Additionally, we compute the quasinormal frequencies of scalar, electromagnetic, and gravitational perturbations in D-dimensional de Sitter spacetime and compare them with previous findings to validate our method.
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    [1] B. P. Abbottet al., Phys. Rev. Lett.116, 061102 (2016) doi:10.1103/PhysRevLett.116.061102
    [2] K. Akiyamaet al. (Event Horizon Telescope Collaboration), Astrophys. J. Lett.875, L1 (2019) doi:10.3847/2041-8213/ab0ec7
    [3] K. D. Kokkotas and B. G. Schmidt, Living Rev. Rel.2, 2 (1999) doi:10.12942/lrr-1999-2
    [4] R. A. Konoplya and A. Zhidenko, Rev. Mod. Phys.83, 793 (2011) doi:10.1103/RevModPhys.83.793
    [5] E. Berti, V. Cardoso, and A. O. Starinets, Class. Quant. Grav.26, 163001 (2009) doi:10.1088/0264-9381/26/16/163001
    [6] J. D. Bekenstein, in2nd International Sakharov Conference on Physics(1996) pp. 216–219, arXiv: gr-qc/9605059 [gr-qc]
    [7] O. Dreyer, B. J. Kelly, B. Krishnanet al., Class. Quant. Grav.21, 787 (2004) doi:10.1088/0264-9381/21/4/003
    [8] V. Cardoso, J. a. L. Costa, K. Destouniset al., Phys. Rev. Lett.120, 031103 (2018) doi:10.1103/PhysRevLett.120.031103
    [9] M. Nozawa and T. Kobayashi, Phys. Rev. D78, 064006 (2008) doi:10.1103/PhysRevD.78.064006
    [10] K. Destounis, R. D. B. Fontana, and F. C. Mena, Phys. Rev. D102, 044005 (2020) doi:10.1103/PhysRevD.102.044005
    [11] R. D. B. Fontana and F. C. Mena, JHEP10, 047 (2022), arXiv: 2203.13933[gr-qc] doi:10.1007/JHEP10(2022)047
    [12] K. Destounis, G. Mascher, and K. D. Kokkotas, Phys. Rev. D105, 124058 (2022) doi:10.1103/PhysRevD.105.124058
    [13] B. Gwak, Eur. Phys. J. Plus138, 582 (2023) doi:10.1140/epjp/s13360-023-04215-7
    [14] W. Xiong and P. C. Li, Phys. Rev. D108, 044064 (2023), arXiv: 2305.04040[gr-qc] doi:10.1103/PhysRevD.108.044064
    [15] Y. Lei, H. Shu, K. Zhanget al., JHEP02, 140 (2024) doi:10.1007/JHEP02(2024)140
    [16] J. Barragán Amado and B. Gwak, JHEP2024, 189 (2024) doi:10.1007/JHEP02(2024)189
    [17] T. Chen, R. G. Cai, and B. Hu, Phys. Rev. D109, 084049 (2024) doi:10.1103/PhysRevD.109.084049
    [18] W. Kinnersley and M. Walker, Phys. Rev. D2, 1359 (1970) doi:10.1103/PhysRevD.2.1359
    [19] J. F. Plebanski and M. Demianski, Annals Phys.98, 98 (1976) doi:10.1016/0003-4916(76)90240-2
    [20] J. B. Griffiths, P. Krtous, and J. Podolsky, Class. Quant. Grav.23, 6745 (2006) doi:10.1088/0264-9381/23/23/008
    [21] S. W. Hawking and S. F. Ross, Phys. Rev. Lett.75, 3382 (1995) doi:10.1103/PhysRevLett.75.3382
    [22] D. Merritt, M. Milosavljevic, M. Favataet al., Astrophys. J. Lett.607, L9 (2004) doi:10.1086/421551
    [23] S. W. Hawking and S. F. Ross, Phys. Rev. D56, 6403 (1997) doi:10.1103/PhysRevD.56.6403
    [24] D. Bini, C. Cherubini, and A. Geralico, J. Math. Phys.49, 062502 (2008) doi:10.1063/1.2938699
    [25] D. Kofroň, Phys. Rev. D92, 124064 (2015) doi:10.1103/PhysRevD.92.124064
    [26] V. P. Frolov, P. Krtouš, and D. Kubizňák, Phys. Rev. D97, 101701 (2018) doi:10.1103/PhysRevD.97.101701
    [27] A. Lopez-Ortega, Gen. Rel. Grav.38, 1565 (2006a) doi:10.1007/s10714-006-0335-9
    [28] A. Lopez-Ortega, Gen. Rel. Grav.38, 743 (2006b) doi:10.1007/s10714-006-0263-8
    [29] A. Lopez-Ortega, Gen. Rel. Grav.44, 2387 (2012) doi:10.1007/s10714-012-1398-4
    [30] A. Jansen, Eur. Phys. J. Plus132, 546 (2017) doi:10.1140/epjp/i2017-11825-9
    [31] K. Destounis, Phys. Lett. B795, 211 (2019) doi:10.1016/j.physletb.2019.06.015
    [32] R. A. Konoplya and A. Zhidenko, Phys. Rev. D106, 124004 (2022) doi:10.1103/PhysRevD.106.124004
    [33] Z. X. Wang and D. R. Guo,Special Functions, (World Scientific, 1989) doi:10.1142/0653
    [34] J. Gray,Linear Differential Equations and Group Theory from Riemann to Poincare, (Birkhäuser Boston, 2008) doi:10.1007/978-0-8176-4773-5
    [35] J. B. Griffiths and J. Podolský,,Exact Space-Times in Einstein's General Relativity, (Cambridge: Cambridge University Press, 2009) doi:10.1017/CBO9780511635397
    [36] M. Abramowitz and I. A. Stegun,Handbook of Mathematical Functions With Formulas, Graphs, and Mathematical Tables, (United States: Government Printing Office, 1965)
    [37] S. A. Teukolsky, Astrophys. J.185, 635 (1973) doi:10.1086/152444
    [38] E. Newman and R. Penrose, J. Math. Phys.3, 566 (1962) doi:10.1063/1.1724257
    [39] J. B. Griffiths and J. Podolsky, Class. Quant. Grav.22, 3467 (2005) doi:10.1088/0264-9381/22/17/008
    [40] E. T. Newman and R. Penrose, J. Math. Phys.7, 863 (1966) doi:10.1063/1.1931221
    [41] H. Suzuki and E. Takasugi, Mod. Phys. Lett. A11, 431 (1996) doi:10.1142/S0217732396000473
    [42] E. Abdalla, K. H. C. Castello-Branco, and A. Lima-Santos, Phys. Rev. D66, 104018 (2002) doi:10.1103/PhysRevD.66.104018
    [43] L. C. B. Crispino, A. Higuchi, and G. E. A. Matsas, Phys. Rev. D63, 124008 (2001) doi:10.1103/PhysRevD.80.029906
    [44] H. Kodama and A. Ishibashi, Prog. Theor. Phys.111, 29 (2004) doi:10.1143/PTP.111.29
    [45] J. Natario and R. Schiappa, Adv. Theor. Math. Phys.8, 1001 (2004) doi:10.4310/ATMP.2004.v8.n6.a4

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Tao Zhou and Peng-Cheng Li. Quasinormal modes of accelerating spacetime[J]. Chinese Physics C, 2025, 49(9): 095104. doi: 10.1088/1674-1137/add10d
Tao Zhou and Peng-Cheng Li. Quasinormal modes of accelerating spacetime[J]. Chinese Physics C, 2025, 49(9): 095104. doi:10.1088/1674-1137/add10d shu
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Received: 2025-03-07
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    Quasinormal modes of accelerating spacetime

      Corresponding author:Peng-Cheng Li,pchli2021@scut.edu.cn
    • School of Physics and Optoelectronics, South China University of Technology, Guangzhou 510641, China
    • Received Date:2025-03-07
    • Available Online:2025-09-15

      Abstract:We calculate the exact values of the quasinormal frequencies for massless perturbations with spin $ s\leq2 $ propagating in purely accelerating spacetime. Using two different methods, we transfer the perturbation equations into hypergeometric differential equations and obtain identical quasinormal frequencies. These purely imaginary spectra are shown to be independent of the spin of the perturbation and match those of the acceleration modes identified in accelerating black holes in the Minkowski limit. This implies that the acceleration modes originate from the purely accelerating spacetime and that the presence of black holes would deform the spectra. Additionally, we compute the quasinormal frequencies of scalar, electromagnetic, and gravitational perturbations inD-dimensional de Sitter spacetime and compare them with previous findings to validate our method.

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