Largescale Structure and the Adhesion Approximation

Details Largescale Structure and the Adhesion Approximation Largescale Structure and the Adhesion Approximation

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.247..260w&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 247, NO.2/NOV15, P. 260, 1990

Astronomy and Astrophysics

Astronomy

89

Scientific paper

The adhesion approximation, introduced by Gurbatov, Saichev & Shandarin, greatly extends the useful range of the Zel'dovich (quasi-linear) approximation by using artificial viscosity to mimic some of the effects of non-linear gravity. We describe a fast, three-dimensional implementation of the adhesion approximation, compare adhesion simulations to N-body calculations with identical initial conditions, and present results from large scale-free and cold dark matter (CDM) initial conditions. The adhesion approximation is generally quite accurate on scales >~2h^-1^Mpc it is most successful for the biased CDM and hot-matter models, while for models with more small-scale power it underestimates the fragmentation of structure into dense clumps. Adhesion simulations with scale-free initial conditions develop a network of filaments, walls, tunnels and cells, with a characteristic size that depends on the amplitude and slope of the power spectrum. Simulated redshift samples drawn from biased CDM simulations show empty voids 20-50 h^-1^Mpc across and walls and filaments up to 150 h^-1^Mpc in length. Unbiased CDM models also show giant superclusters, but their underdense regions typically contain a sprinkling of isolated galaxies. Non-linear gravitational evolution resembles, in some respects, a 'smoothing' process that acts on the initial density fluctuations. As time increases, larger scale modes of the density field come to dominate the evolved structure; finer details are washed away by merging, and gravitational collapse transfers energy from ordered motions into virial velocity dispersions. Sheets and filaments develop directly from features present in the initial conditions. The combination of gravitational instability and biasing in hierarchical models like cold dark matter creates a network of structure with a remarkable resemblance to the observed galaxy distribution.

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