Decay of a charged scalar field around a black hole: Quasinormal modes of RN, RNAdS, and dilaton black holes

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 66, Issue 8, 2002, Pages

  Konoplya, R A ^a  

^a OLES HONCHAR DNIPRO NATIONAL UNIVERSITY   (Ukraine)

Author keywords

[No Author keywords available]

Indexed keywords

ACCELERATION; ARTICLE; BLACK HOLE; CALCULATION; COSMOLOGICAL PHENOMENA; ELECTROMAGNETIC RADIATION; GRAVITY; MASS; MATHEMATICAL ANALYSIS; MATHEMATICS; OSCILLATION; TIME;

EID: 3543020738     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.66.084007     Document Type: Article

References (28)

1. K. Kokkotas and B. Schmidt, in Living Reviews in Relativity: www.livingreviews.org (1999).
2. J. Maldacena, Adv. Theor. Math. Phys. 2, 231 (1998).
3. G.T. Horowitz and V. Hubeny, Phys. Rev. D 62, 024027 (2000).
4. V. Cardoso and J.P.S. Lemos, Phys. Rev. D 63, 124015 (2001).
5. V. Cardoso and J.P.S. Lemos, Phys. Rev. D 64, 084017 (2001).
6. V. Cardoso and J.P.S. Lemos, Phys. Rev. D 66, 064006 (2002).
7. D. Birmingham, I. Sachs, and S.N. Solodukhin, Phys. Rev. Lett. 88, 151301 (2002).
8. B. Wang, C.Y. Lin, and E. Abdalla, Phys. Lett. B 481, 79 (2000).
9. B. Wang, C.M. Mendes, and E. Abdalla, Phys. Rev. D 63, 084001 (2001).
10. I.G. Moss and J.P. Norman, Class. Quantum Grav. 19, 2323 (2002).
11. P. Brady, C. Chambers, W. Krivan, and P. Laguna, Phys. Rev. D 55, 7538 (1997).
12. P. Brady, C. Chambers, W. Laarakkers, and E. Poison, Phys. Rev. D 60, 064003 (1999).
13. R. Price, Phys. Rev. D 5, 2419 (1972).
14. S. Hod and T. Piran, Phys. Rev. D 58, 024017 (1998).
15. The point is that the WKB QNM’s for (Formula presented) (Formula presented) are monotonically decreasing with increasing Q. Unfortunately, the WKB method, being quite accurate for higher multipole index l (it practically coincides with numerical results for (Formula presented) may give considerable error for (Formula presented) modes. Yet even for the neutral scalar field around the RN BH the QN modes were not computed with a more acuurate method as far as we are aware. Thus one cannot be sure that when computing these modes with the help of numerical methods the quasinormal behavior will be the same.
16. S. Iyer and C.M. Will, Phys. Rev. D 35, 3621 (1987).
17. S. Iyer, Phys. Rev. D 35, 3632 (1987).
18. R.A. Konoplya, Phys. Rev. D 66, 044009 (2002).
19. C.F.E. Holzhey and F. Wilczek, Nucl. Phys. B298, 447 (1992).
20. R. Moderski and M. Rogatko, Phys. Rev. D 63, 084014 (2001).
21. V. Ferrari, M. Pauri, and F. Piazza, Phys. Rev. D 63, 064009 (2001).
22. R.A. Konoplya, Gen. Relativ. Gravit. 34, 329 (2002).
23. S. Hod and T. Piran, Phys. Rev. D 55, 3485 (1997).
24. M.W. Choptuik, Phys. Rev. Lett. 70, 9 (1993).
25. W.T. Kim and J.J. Oh, Phys. Lett. B 514, 155 (2001).
26. D. Birmingham, Phys. Rev. D 64, 064024 (2001).
27. M. Spradlin and A. Strominger, J. High Energy Phys. 11, 021 (1999).
28. L. Xue, B. Wang, and R-K. Su, Phys. Rev. D 66, 024032 (2002).