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A 48 T. PADMANABHAN are less than unity. Mathematically, this can be understood from the evolution equations for the density contrast - written in fourier space as : (28) where t5k(t) is the fourier transform of the density contrast, j5 is the background density and Q is a nonlocal, nonlinear function which couples the mode k to all other modes k' (Peebles, 1980). Coupling between different modes is significant in two cases. The obvious case is one with 15k ;::: 1. A more interesting possibility arises for modes with no initial power [or exponentially small power].

PADMANABHAN e We know that, in the linear regime, = eL ex a2 . Equation (13) shows that, in the quasilinear regime, = eQL ex a6/(n+4). Spectra with n < -1 grow faster than a 2 , spectra with n > -1 grow slower than a 2 and n = -1 spectrum grows as a 2 . Direct algebra shows that e - - ~Qda,x) ex [~L(a,l)] 3 (14) reconfirming the local dependence in a and nonlocal dependence in spatial coordinate. This result has no trace of original assumptions [spherical evolution, scale-invariant spectrum ....

1996. HST-2, Proceedings of the Second European Symposium on the Hubble Space Telescope (eds. P. Benvenuto, F. Macchetto & E. Schreier), (in press). SCHADE, D. 1996. HST-2, Proceedings of the Second European Symposium on the Hubble Space Telescope (eds. P. Benvenuto, F. Macchetto & E. Schreier), (in press ). , LE FtvRE, O. & TRESSE, 1. (1995). ApJ, 451, Ll. , PETTINI, M. & HAMILTON, D. (1995). AJ, 110, 2519. , DICKINSON, M. L. (1996). C. & HAMILTON, D. (1992). AJ, 104, 94l. C. & HAMILTON, D. (1993).

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