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10
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84927270514
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see, however, H. M. Hodges, J. Silk, and M. S. Turner, Fermilab Report No. 87/153-A, 1987 (unpublished).
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12
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84927270513
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Ya. B. Zel'dovich, A. A. Ruzmaikin, and D. D. Sokoloff, Magnetic Fields in Astrophysics (Gordon and Breach, New York, 1983).
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13
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84927270512
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Q. J. R. Astron. Soc. (to be published, 1988).
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Rees, M.J.1
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23
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84927270511
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The energy density in photons is ργ= π2T4/ 15. The energy density in photons varies as gstar-4/3a-4, i.e., only precisely as a-4 when the effective number of degrees of freedom of the relativistic particles in thermal equilibrium with the photons gstar is constant. For present purposes it is sufficient to ignore the slight gstar dependence.
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28
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35949009476
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Superadiabatic amplification seems to have been first discussed in the context of gravitons (see Ref. 20). The equations of motion for the graviton in a flat FRW cosmology are identical to that for a minimally coupled scalar field, so it applies there as well. Superadiabatic amplification as a means of particle production in the context of inflation is discussed in detail by
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(1988)
Phys. Rev. D
, vol.37
, pp. 2743
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Turner, M.S.1
Widrow, L.M.2
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41
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84927270510
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L. F. Abbott, in Quark Matter '84, proceedings of the Fourth International Conference on Ultrarelativistic Nucleus-Nucleus Collisions, Helsinki, Finland, 1987, edited by K. Kajantie (Lecture Notes in Physics, Vol. 221) (Springer, New York, 1985);
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43
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0001422612
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During the reheating (or coherent oscillation) phase the temperature of the Universe at first rapidly rises to ( MTRH)1/2 and then falls as t-1/4, reaching a temperature of TRH when the Universe becomes radiation dominated. For a detailed discussion of reheating, see Ref. 15, or
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(1983)
Phys. Rev. D
, vol.28
, pp. 1243
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Turner, M.S.1
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55
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84927270509
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Throughout we will assume that all quantum fields in de Sitter space are excited, with an energy density of the order of ( H / 2 π )4, as conjected by Gibbons and Hawking (Ref. 24). For a minimally coupled scalar field it is well established that any comoving observer will detect a thermal bath of particles with the Gibbons-Hawking temperature, H / 2 pi [see Refs. 24 and 25, and N. D. Birrell and P. C. W. Davies, Quantum Fields in Curved Space (Cambridge University Press, Cambridge, England, 1982)]. Furthermore, Birrell and Davies have shown that in de Sitter space, a massless, conformally coupled scalar field will have nonthermal fluctuations with an energy density of the order of H4. However, for conformally coupled fields there are some who would argue that this should not be the case, as the equations of motion are just those of a free field in Minkowski space. While this is certainly true, the boundary conditions are very different, and it is boundary conditions which give rise to Hawking radiation for black holes and accelerated observers. To our knowledge, the issue has not been definitely resolved. In any case, in the situations of interest to us the fields are not conformally coupled.
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56
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In ``ordinary inflation,'' gamma changes from apeq - 1 to 0 as the Universe goes from the de Sitter phase to the reheating phase (coherent field oscillations), and one might have hoped that during the transition, when gamma is
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58
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Radiatively induced spontaneous symmetry breaking and phase transitions in curved spacetime
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(1980)
Annals of Physics
, vol.128
, pp. 376
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Shore, G.M.1
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