真空无奇点黑洞的拟正则模:无质量标量场扰动
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摘要
研究带有de Sitter中心的球对称黑洞在标量场扰动下的拟正则模.几何上来讲,这种黑洞在半径r很大的时候趋近与史瓦西解形式,在r趋于0的时候是de Sitter解形式的.在这里通过变化参数r0(它与宇宙学常数有关),角量子数l,泛音数n和黑洞质量M来研究这个黑洞的拟正则模ω.计算结果发现:拟正则模在随r0的变化出现极大值和极小值,同时对于一定范围的r0,当拟正则模随泛音数n变化时也会出现极值现象,这是值得关注的.
In this paper,we investigate quasinormal mode( QNM) of the spherically symmetric BH with de Sitter centre due to scalar perturbations. This BH is,geometrically,asymptotically Schwarzschild for large r and asymptotically de Sitter as r → 0. We analyze the QNM ω by varying the parameter r0( it is related to cosmological constant),spherical harmonic index l,overtune n and the BH mass M. According to calculations,we find that the QNM Lhave maximum and minimum with a changing r0,and for some r0 it is worthy to attention that the QNM have extreme with a changing overtune n
In this paper,we investigate quasinormal mode( QNM) of the spherically symmetric BH with de Sitter centre due to scalar perturbations. This BH is,geometrically,asymptotically Schwarzschild for large r and asymptotically de Sitter as r → 0. We analyze the QNM ω by varying the parameter r0( it is related to cosmological constant),spherical harmonic index l,overtune n and the BH mass M. According to calculations,we find that the QNM Lhave maximum and minimum with a changing r0,and for some r0 it is worthy to attention that the QNM have extreme with a changing overtune n
引文
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[14]FERNANDO S,CORREA J.Quasinormal modes of the Bardeen black hole:Scalar perturbations[J].Phys Rev D,2012,86:064039.
[2]BARDEEN J M.Proceedings of GR5[M].USSR:Tbilisi,1968.
[3]AYN-BEATO E,GARCA A.The Bardeen Model as a Nonlinear Magnetic Monopole[J].Physics Letters B,2000,493(1-2):149-152.
[4]DYMNIKOVA I.Vacuum Nonsingular Black Hole[J].Gen Relativ Gravit,1992,24:235-242.
[5]LI X Z,HAO J G,LIU D J.Quasinormal modes of string black hole[J].Phy Lett B,2001,507:312-361.
[6]LIU D J,YANG B,ZHAI Y J,et al.Quasinormal modes for asymptotic safe black holes[J].Class Quantum Gravity,2012,29:145009.
[7]NOLLERT H P.Quasinormal modes:the characteristic'sound'of black holes and neutron stars[J].Class Quantum Gravity,1999,16:159-216.
[8]BERTI E,CARDOSO V,STARINETS A O.Quasinormal modes of black holes and black branes[J].Classical Quantum Gravity,2009,26:163001.
[9]HOD S.Bohr's Correspondence Principle and the Area Spectrum of Quantum Black Holes[J].Phys Rev Lett,1998,81:4293-4296.
[10]KONOPLYA R A,ZHIDENKO A.Quasinormal modes of black holes:From astrophysics to string theory[J].Rev Mod Phys,2011,83(3):793-836.
[11]KONOPLYA L R A.Quasinormal behavior of the D-dimensional Schwarzschild black hole and the higher order WKB approach[J].Phys Rev D,2003,68:024018.
[12]CHANDRASEKHAR S.The Mathematical Theory of Black Holes[M].London:Oxford University Press,1992.
[13]IYER S,WILL C M.Black-hole normal modes:A WKB approach.I.Foundations and application of a higher-order WKB analysis of potential-barrier scattering[J].Phys Rev D,1987,35(12):3621-3631.
[14]FERNANDO S,CORREA J.Quasinormal modes of the Bardeen black hole:Scalar perturbations[J].Phys Rev D,2012,86:064039.