Filamentary and hierarchical pictures - Kinetic energy criterion

Details Filamentary and hierarchical pictures - Kinetic energy criterion Filamentary and hierarchical pictures - Kinetic energy criterion

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...399..397k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 399, no. 2, p. 397-404.

Astronomy and Astrophysics

Astrophysics

16

Astronomical Models, Galactic Clusters, Galactic Evolution, Kinetic Energy, Dark Matter, Velocity Distribution

Scientific paper

We present a new criterion for formation of second-generation filaments. The criterion called the kinetic energy ratio, KR, is based on comparison of peculiar velocities at different scales. We suggest that the clumpiness of the distribution in some cases might be less important than the 'coldness' or 'hotness' of the flow for formation of coherent structures. The kinetic energy ratio is analogous to the Mach number except for one essential difference. If at some scale KR is greater than 1, as estimated at the linear stage, then when fluctuations of this scale reach nonlinearity, the objects they produce must be anisotropic ('filamentary'). In the case of power-law initial spectra the kinetic ratio criterion suggests that the border line is the power-spectrum with the slope n = -1.

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