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The power spectrum P(k)\propto k^n with n=-2 is close to the shape of themeasured galaxy spectrum on small scales. Unfortunately this spectrum hasproven rather difficult to simulate. Further, 2-dimensional simulations havesuggested a breakdown of self-similar scaling for spectra with n<-1 due todivergent contributions from the coupling of long wave modes. This paper is thesecond (numerical) part of our investigation into the nonlinear gravitationalclustering of scale-free spectra. Using high-resolution N-body simulations wefind that the n=-2 power spectrum, as well as trajectories of the amplitude andphase of Fourier modes, display self-similar scaling. The evolution of thephase shift does show a different scaling at late times, but this was shownanalytically to arise from the purely kinematical effect of bulk flows. Thusour analytical and N-body results verify that self-similarity in gravitationalclustering holds for -3<n<1. The N-body spectrum is also compared with analyticfitting formulae, which are found to slightly underestimate the power in thenonlinear regime. The asymptotic shape of the spectrum at high-k is a power lawwith the same slope as predicted by the stable clustering hypothesis.Comment: 34 pages, 14 figures included. Accepted for publication in the  Astrophysical Journa

Self‐Similar Evolution of Gravitational Clustering. II.N‐Body Simulations of then= −2 Spectrum