A method is presented for computing the mass distribution that develops in a model universe with no characteristic lengths provided by the matter or by the background expanding cosmological model. This problem is of interest as a possible approximation to our universe and as a test of our ability to compute the evolution of the mass distribution in an expanding universe. A preliminary application of the method yields results intermediate between what has been obtained from conventional N-body models and what followed from the Davis-Peebles (1983) integration of the BBGKY hierarchy: the mass autocorrelation function xi(r) approaches the expected power-law behavior at small lag r, but xi(r) breaks below the power law at a value of xi larger than that suggested by the galaxy clustering data.
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P. J. E. Peebles (1985) studied this question.