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Referencias:

• Vilenkin, A., (1989) Phys. Rev. D, 39, p. 1116
• Kuchar, K., (1982) Quantum Gravity 2, A Second Oxford Symposium, 1981, p. 329. , edited by, C. J. Isham, Oxford University Press, Oxford
• Hawking, S., (1979) General Relativity, p. 746. , edited by, S. Hawking, W. Israel, Cambridge University Press, Cambridge, England
• Hartle, J., Hawking, S., (1983) Phys. Rev. D, 28, p. 2960
• Hartle, J., (1985), Yale University; J. Hartle, in Gravitation and Astrophysics (Cargese, 1986), proceedings of the NATO Advanced Study Institute, Cargese, France, 1986, edited by B. Carter and J. B. Hartle (NATO ASI Series B, Vol. 156) (Plenum, New York, 1987); B. DeWitt, in Quantum Gravity, proceedings of the Third Seminar, Moscow, 1984, edited by M. A. Markov, V. A. Berezin, and V. P. Frolov (World Scientific, Singapore, 1985), p. 103; Anderson, A., DeWitt, B., (1986) Found. Phys., 16, p. 91
• Castagnino, M., (1971) J. Math. Phys., 12, p. 2203
• Ehlers, J., (1973) Relativity, Astrophysics and Cosmology, p. 1. , edited by, W. Israel, Reidel, Dordrecht
• Castagnino, M., Harari, D., (1982) Rev. Union Mat. Argent., 30, p. 147
• As in the case of gauge theories, or the possibility of wormholes connecting different zones of the Universe; Halliwell, J.J., Hawking, S.W., (1985) Phys. Rev. D, 31, p. 1777
• D'Eath, P.D., Halliwell, J.J., Cambridge University report, 1986 (unpublished); Hartle, J., (1988) Phys. Rev. D, 37, p. 2818
• Castagnino, M., Proceedings of the Friedmann Commemoration Conference, Leningrad, 1988
• Thurston, W.P., (1988) Ann. Math., 124, p. 203
• Monogue, C.A., Copeland, E., Dray, T., report, 1988 (unpublished); Hawking, S.W., (1985) Phys. Rev. D, 32, p. 2489
• Kazama, Y., Nakayama, R., (1985) Phys. Rev. D, 32, p. 2500
• DeWitt, B.S., (1967) Phys. Rev., 160, p. 1113
• (1986) S. W. Hawking and D. N. Page, Nucl. Phys., 264 B, p. 185. , This result essentially follows also from the fact that in the semiclassical limit the probability of finding the configuration within a region of superspace is proportional to the classical time that the classical solution spends in that region
• From Eq. (5.11) these equations yield < ψ , ψ > =1, i.e., the original normalization (3.6); Vilenkin, A., (1988) Phys. Rev. D, 37, p. 888. , The oscillating factor could be different if we use, e.g., the Vilenkin tunneling boundary condition, but the prefactor is the same [cf., ]. In both cases the oscillating factor is averaged. This fact shows that, even if in the case of the Hartle-Hawking boundary condition, we are not in the case of Eq. (5.1) (because we have a sum of two terms) the conclusion about probabilistic time, in the classical limit, remains valid
• Castagnino, M., Proceedings of the Fourth Seminar on Quantum Gravity, Moscow, 1987, , (World Scientific, Singapore, to be published)
• Castagnino, M., (1988) Proceedings of SILARG VI, Rio de Janeiro, 1987, , World Scientific, Singapore

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