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3
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85038282888
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see also B. Chaboyer et al., astro-ph/9706128, with new results based on recent Hipparcos parallax measurements which indicate younger ages (Formula presented) smaller) for the oldest globular clusters. If these results are confirmed the age problem will possibly be weakened.
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Chaboyer, B.1
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4
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85038281548
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However, it is still early to say that the age crisis has gone away (see, e.g., W. L. Freedman, in astro-ph/9706072 for a recent discussion on this and related topics).
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Freedman, W.L.1
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8
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3242696829
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M. Hamuy et al., Astron. J. 112, 2398 (1996).
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Astron. J.
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Hamuy, M.1
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10
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0000878495
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K. Freese et al., B287, 797 (1987);
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(1987)
, vol.B287
, pp. 797
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Freese, K.1
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18
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85038280851
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For the models considered in this paper (Formula presented) is negligibly small during nucleosynthesis. However, this is not necessarily true for all (Formula presented)-decaying models present in the literature. For instance, for a class of models in which (Formula presented)=const, Freese et al. 4
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For the models considered in this paper (Formula presented) is negligibly small during nucleosynthesis. However, this is not necessarily true for all (Formula presented)-decaying models present in the literature. For instance, for a class of models in which (Formula presented)=const, Freese et al. 4 showed that standard primordial nucleosynthesis constraints the parameter (Formula presented) to be (Formula presented).
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31
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85038270270
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The evolution of modes bigger than the Hubble radius is described by the general relativistic equations [see, e.g., T. Padmanabhan, Structure Formation in the Universe, (Cambridge University Press, Cambridge, England, 1993), pp. 141–146]. Since nonrelativistic matter is conserved, and assuming that the (Formula presented) component is smooth the relativistic equation for (Formula presented) may be written as an equation for (Formula presented), giving us the same Newtonian equation used to describe the evolution of modes inside the horizon
-
The evolution of modes bigger than the Hubble radius is described by the general relativistic equations [see, e.g., T. Padmanabhan, Structure Formation in the Universe, (Cambridge University Press, Cambridge, England, 1993), pp. 141–146]. Since nonrelativistic matter is conserved, and assuming that the (Formula presented) component is smooth the relativistic equation for (Formula presented) may be written as an equation for (Formula presented), giving us the same Newtonian equation used to describe the evolution of modes inside the horizon.
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36
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0002641716
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M. Hamuy et al., Astron. J. 109, 1 (1995);
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Astron. J.
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, pp. 1
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Hamuy, M.1
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37
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0000007419
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M. Hamuy et al., 112, 2391 (1996).
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(1996)
, vol.112
, pp. 2391
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Hamuy, M.1
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43
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0000723834
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A. J. Surdej et al., 105, 2064 (1993);
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(1993)
, vol.105
, pp. 2064
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Surdej, A.J.1
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44
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0003000840
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edited by J. Surdej, D. Fraipont-Caro, E. Gosset, S. Refsdal, and M. Remy (University of Liege, Liege, 1994), p. 127
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E. E. Falco, in Gravitational Lenses in the Universe, edited by J. Surdej, D. Fraipont-Caro, E. Gosset, S. Refsdal, and M. Remy (University of Liege, Liege, 1994), p. 127;
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Gravitational Lenses in the Universe
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Falco, E.E.1
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