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Chaos in Relativity and Cosmology

Published online by Cambridge University Press:  12 April 2016

G. Contopoulos ,
N. Voglis  and
C. Efthymiopoulos
G. Contopoulos
Affiliation:
Research Center for Astronomy, Academy of Athens Department of Astronomy, University of Athens
N. Voglis
Affiliation:
Department of Astronomy, University of Athens
C. Efthymiopoulos
Affiliation:
Research Center for Astronomy, Academy of Athens Department of Astronomy, University of Athens

Abstract

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Chaos appears in various problems of Relativity and Cosmology. Here we discuss (a) the Mixmaster Universe model, and (b) the motions around two fixed black holes, (a) The Mixmaster equations have a general solution (i.e. a solution depending on 6 arbitrary constants) of Painlevé type, but there is a second general solution which is not Painlevé. Thus the system does not pass the Painlevé test, and cannot be integrable. The Mixmaster model is not ergodic and does not have any periodic orbits. This is due to the fact that the sum of the three variables of the system (α + β + γ) has only one maximum for τ = τm and decreases continuously for larger and for smaller τ. The various Kasner periods increase exponentially for large τ. Thus the Lyapunov Characteristic Number (LCN) is zero. The “finite time LCN” is positive for finite τ and tends to zero when τ → ∞. Chaos is introduced mainly near the maximum of (α + β + γ). No appreciable chaos is introduced at the successive Kasner periods, or eras. We conclude that in the Belinskii-Khalatnikov time, τ, the Mixmaster model has the basic characteristics of a chaotic scattering problem, (b) In the case of two fixed black holes M1 and M2 the orbits of photons are separated into three types: orbits falling into M1 (type I), or M2 (type II), or escaping to infinity (type III). Chaos appears because between any two orbits of different types there are orbits of the third type. This is a typical chaotic scattering problem. The various types of orbits are separated by orbits asymptotic to 3 simple unstable orbits. In the case of particles of nonzero rest mass we have intervals where some periodic orbits are stable. Near such orbits we have order. The transition from order to chaos is made through an infinite sequence of period doubling bifurcations. The bifurcation ratio is the same as in classical conservative systems.

Type
Cosmology
Information
International Astronomical Union Colloquium , Volume 172: Impact of Modern Dynamics in Astronomy , 1999 , pp. 1 - 16
Copyright
Copyright © Kluwer 1999

References

Ablowitz, M.J., Ramani, A. and Segur, H.:1980, J.Math.Phys., 21, 715.Google Scholar
Barrow, J.D., and Levin, J.: 1998, Phys. Rev. Lett., 80, 656.Google Scholar
Belinskii, V.A. and Khalatnikov, I.M.: 1969, Sov.Phys.JETP, 29, 911.Google Scholar
Benettin, G., Cercignani, C., Galgani, L. and Giorgilli, A.: 1980, Lett. Nuovo Cim., 28, 1.CrossRefGoogle Scholar
Bombelli, L. and Calzetta, E.: 1992, Class. Quantum Grav., 9, 2573.CrossRefGoogle Scholar
Calzetta, E. and El Hasi, C.: 1993, Class. Quantum Grav., 10, 1825.Google Scholar
Chicone, C., Mashhoon, B. and Retzloff, D.G.: 1997, Class. Quantum Grav., 14, 699.Google Scholar
Christiansen, F., Rugh, H.H. and Rugh, S.E.: 1995, J.Phys.A, 28, 657.Google Scholar
Contopoulos, G.: 1990, Proc.R.Soc.Lond. A, 431, 183.Google Scholar
Contopoulos, G.: 1991, Proc.R.Soc.Lond. A, 435, 551.Google Scholar
Contopoulos, G., Grammaticos, B. and Ramani, A.: 1993, J.Phys.A, 26, 5795.Google Scholar
Contopoulos, G., Grammaticos, B. and Ramani, A.: 1995, J.PhysA, 28, 5313.Google Scholar
Cornish, N.J. and Gibbons, G.W.: 1997, Class. Quantum Grav., 14, 1865.CrossRefGoogle Scholar
Cornish, N.J. and Levin, J.J.: 1997, Phys. Rev. Lett.,88, 998.Google Scholar
Cornish, N.J. and Levin, J.J.: 1998, Phys. Rev. D, 55, 7489.Google Scholar
Cornish, N.J. and Shellard, E.P.S.: 1998,Phys. Rev. Lett., 81, 3571.CrossRefGoogle Scholar
Cushman, R. and Sniatycki, J.: 1995, Rep.Math.Phys., 36, 75.Google Scholar
Darian, B.K. and Künzle, H.P.: 1996, Class. Quantum Grav., 13, 2651.CrossRefGoogle Scholar
Dettmann, C.P., Frankél, N.E. and Cornish, N.J.: 1994, Phys. Rev. D, 50, R618.CrossRefGoogle Scholar
Drake, S.P., Dettmann, C.P., Frankél, N.E. and Cornish, N.J.: 1996, Phys.Rev. E, 53, 1351.CrossRefGoogle Scholar
Hobill, D., Bernstein, D., Simpkins, D. and Welge, M.: 1992, Class. Quantum Grav., 8, 1155.Google Scholar
Hobill, D., Burd, A. and Coley, A. (eds): 1994, Deterministic Chaos in General Relativity, Plenum Press, N. York.Google Scholar
Khalatnikov, I.M., Lifshitz, E.M., Khanin, K.M., Shchur, I.N. and Sinai, Ya.G.: 1985, J.Stat.Phys., 38, 97.Google Scholar
Landau, L.D., and Lifshitz, E.M.: 1971, The Classical Theory of Fields, Pergamon Press, Oxford.Google Scholar
Latifi, A., Musette, M. and Conte, R.: 1994, Phys.Lett. A,194, 83.Google Scholar
Letelier, P.S. and Vieira, W.M.: 1997,Class. Quantum Grav., 14, 1249.CrossRefGoogle Scholar
Majumdar, S.D.: 1947, Phys. Rev., 72, 390.CrossRefGoogle Scholar
Misner, C.M.: 1969,Phys. Rev. Lett., 22, 1071.Google Scholar
Misner, C.M., Thorne, K. and Wheeler, J.A.: 1977, Gravitation, Freeman, San Francisco.Google Scholar
Papapetrou, A.: 1947, Proc. R. Irish Acad., 51, 191.Google Scholar
Podolsky, J. and Vesely, K.: 1998, Phys. Rev. D,58, 081501.Google Scholar
Poincaré, H.: 1892, Les Méthodes Nouvelles de la Mécanique Céleste, I, Gauthier Villars, Paris.Google Scholar
Raychaudhuri, A.: 1955, Phys.Rev., 98, 1123.Google Scholar
Rugh, S.E. and Jones, B.J.T.: 1990, Phys.Lett. A,47, 353.CrossRefGoogle Scholar
Smith, H. and Contopoulos, G.: 1996, Astron. Astrophys., 314, 795.Google Scholar
Suzuki, S. and Maeda, K.: 1997,Phys. Rev. D, 55, 4848.CrossRefGoogle Scholar
Szydlowski, M.: 1997, Gen.Rev.Grav., 29, 185.CrossRefGoogle Scholar
Taub, A.H.: 1951, Ann.Math., 53, 472.Google Scholar
Varvoglis, H. and Papadopoulos, D.: 1991, Astron. Astrophys., 261, 664.Google Scholar
Voglis, N. and Contopoulos, G.: 1994, J.Phys.A, 27, 4899.Google Scholar
Yurtsever, U.: 1995,Phys. Rev. D, 52, 3176.Google Scholar