Theoretical and Mathematical Physics

, Volume 170, Issue 1, pp 71–82 | Cite as

Classical analogue of a quantum Schwarzschild black hole: “Standard model” and beyond

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Abstract

We build a model in which the main global properties of classical and semiclassical black holes become local: these are the event horizon, “no-hair,” temperature, and entropy. Our construction is based on the features of a quantum collapse, discovered when studying some particular quantum black hole models. But our model is purely classical, and this allows using the Einstein equations and classical (local) thermodynamics self-consistently and, in particular, solving the “puzzle of log 3.”

Keywords

quantum black hole thermodynamics quasinormal frequency 
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References

  1. 1.
    S. W. Hawking and G. F. R. Ellis, The Large Scale Structure of Space-Time (Cambridge Monogr. Math. Phys., Vol. 1), Cambridge Univ. Press, London (1973).MATHCrossRefGoogle Scholar
  2. 2.
    R. Ruffini and J. A. Wheeler, Phys. Today, 24, 30–36 (1971).ADSCrossRefGoogle Scholar
  3. 3.
    T. Regge and J. A. Wheeler, Phys. Rev., 108, 1063–1069 (1957).MathSciNetADSMATHCrossRefGoogle Scholar
  4. 4.
    S. Chandrasekhar, The Mathematical Theory of Black Holes (Intl. Series Monogr. Phys., Vol. 69), Oxford Univ. Press, New York (1983).MATHGoogle Scholar
  5. 5.
    D. Cristodoulou, Phys. Rev. Lett., 25, 1596–1597 (1970).ADSCrossRefGoogle Scholar
  6. 6.
    D. Cristodoulou and R. Ruffini, Phys. Rev. D, 4, 3552–3555 (1971).ADSCrossRefGoogle Scholar
  7. 7.
    J. D. Bekenstein, Lett. Nuovo Cimento, 4, 737–740 (1972); Phys. Rev. D, 7, 2333–2346 (1973); 9, 3292–3300 (1974).ADSCrossRefGoogle Scholar
  8. 8.
    J. M. Bardeen, B. Carter, and S. W. Hawking, Commun. Math. Phys., 31, 161–170 (1973).MathSciNetADSMATHCrossRefGoogle Scholar
  9. 9.
    S. W. Hawking, Nature, 248, 30–31 (1974); Commun. Math. Phys., 43, 199–220 (1975).ADSCrossRefGoogle Scholar
  10. 10.
    W. G. Unruh, Phys. Rev. D, 14, 870–892 (1976).ADSCrossRefGoogle Scholar
  11. 11.
    J. D. Bekenstein, Lett. Nuovo Cimento, 11, 467–470 (1974).ADSCrossRefGoogle Scholar
  12. 12.
    J. D. Bekenstein and V. F. Mukhanov, Phys. Lett. B, 360, 7–12 (1995); arXiv:gr-qc/9505012v1 (1995).MathSciNetADSCrossRefGoogle Scholar
  13. 13.
    A. Ashtekar, J. Baez, A. Corichi, and K. Krasnov, Phys. Rev. Lett., 80, 904–907 (1998); arXiv:gr-qc/9710007v1 (1997).MathSciNetADSMATHCrossRefGoogle Scholar
  14. 14.
    A. Ashtekar, J. Baez, and K. Krasnov, Adv. Theor. Math. Phys., 4, 1–94 (2000).MathSciNetMATHGoogle Scholar
  15. 15.
    S. Hod, Phys. Rev. Lett., 81, 4293–4296 (1998); arXiv:gr-qc/9812002v2 (1998).MathSciNetADSMATHCrossRefGoogle Scholar
  16. 16.
    L. Motl, Adv. Theor. Math. Phys., 6, 1135–1162 (2003); arXiv:gr-qc/0212096v3 (2002).MathSciNetGoogle Scholar
  17. 17.
    L. Motl and A. Neitzke, Adv. Theor. Math. Phys., 7, 307–330 (2003).MathSciNetGoogle Scholar
  18. 18.
    J. Natario and R. Schiappa, Adv. Theor. Math. Phys., 8, 1001–1131 (2004); arXiv:hep-th/0411267v3 (2004).MathSciNetMATHGoogle Scholar
  19. 19.
    V. A. Berezin, Phys. Lett. B, 241, 194–200 (1990).MathSciNetADSCrossRefGoogle Scholar
  20. 20.
    V. A. Berezin, A.M. Boyarsky, and A. Yu. Neronov, Phys. Rev. D, 57, 1118–1128 (1998); arXiv:gr-qc/9708060v1 (1997).MathSciNetADSCrossRefGoogle Scholar
  21. 21.
    V. A. Berezin and M. Yu. Okhrimenko, Class. Q. Grav., 18, 2195–2215 (2001); arXiv:gr-qc/0006085v1 (2000).MathSciNetADSMATHCrossRefGoogle Scholar

Copyright information

© Pleiades Publishing, Ltd. 2012

Authors and Affiliations

  1. 1.Institute for Nuclear ResearchRASMoscowRussia

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