Scale-Invariant Correlation Functions of Cosmological Density Fluctuations in the Strong Clustering Regime

Details Scale-Invariant Correlation Functions of Cosmological Density Fluctuations in the Strong Clustering Regime Scale-Invariant Correlation Functions of Cosmological Density Fluctuations in the Strong Clustering Regime

1996-05-08

arxiv.org/abs/astro-ph/9605032v1

Astronomy and Astrophysics

Astrophysics

24 pages, no figures, uses aaspp4.sty, Submitted to ApJ

Scientific paper

10.1086/304618

We have investigated the scale-invariant solutions of the BBGKY equations for spatial correlation functions of cosmological density fluctuations and the mean relative peculiar velocity in the strongly nonlinear regime. It is found that the solutions for the mean relative physical velocity depend on the three-point spatial correlation function and the skewness of the velocity fields. We find that the stable condition in which the mean relative physical velocity vanishes on the virialized regions is satisfied only under the assumptions which Davis \& Peebles took in his paper. It is found, however, that their assumptions may not be general in real. The power index of the two-point correlation function in the strongly nonlinear regime depends on the mean relative peculiar velocity, the three-point correlation function and the skewness. If the self-similar solutions exist, the power index in the strongly nonlinear regime is related to the power index of the initial power spectrum and its relation depends on the three-point correlation function and the skewness through the mean relative peculiar velocity. Furthermore it is found that the mean relative physical velocity should have the values between 0 and the Hubble expanding velocity. When the mean relative physical velocity equals to the Hubble expanding velocity, there might exist self-similar solutions in which the power index of the two-point correlation function in the strongly nonlinear regime is independent of the initial power index $n$.

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