TY - JOUR
T1 - Emergence of filamentary structure in cosmological gravitational clustering
AU - Sathyaprakash, B. S.
AU - Sahni, Varun
AU - Shandarin, Sergei F.
PY - 1996
Y1 - 1996
N2 - The morphological nature of structures that form under gravitational instability has been of central interest to cosmology for over two decades. A remarkable feature of large-scale structures in the universe is that they occupy a relatively small fraction of the volume and yet show coherence on scales comparable to the survey size. With the aid of a useful synthesis of percolation analysis and shape statistics we explore the evolution of morphology of isolated density clumps in real space, and that of the cluster distribution as a whole, in scale-invariant cosmological models of gravitational instability. Our results, based on an exhaustive statistical analysis, indicate that at finite density thresholds one-dimensional filaments are more abundant than two-dimensional sheets (pancakes) at most epochs and for all spectra, although the first singularities could be pancake-like. Both filamentarity and pancakeness of structures grow with time (in scale-free models this is equivalent to an increase in resolution), leading to the development of a long coherence length scale in simulations.
AB - The morphological nature of structures that form under gravitational instability has been of central interest to cosmology for over two decades. A remarkable feature of large-scale structures in the universe is that they occupy a relatively small fraction of the volume and yet show coherence on scales comparable to the survey size. With the aid of a useful synthesis of percolation analysis and shape statistics we explore the evolution of morphology of isolated density clumps in real space, and that of the cluster distribution as a whole, in scale-invariant cosmological models of gravitational instability. Our results, based on an exhaustive statistical analysis, indicate that at finite density thresholds one-dimensional filaments are more abundant than two-dimensional sheets (pancakes) at most epochs and for all spectra, although the first singularities could be pancake-like. Both filamentarity and pancakeness of structures grow with time (in scale-free models this is equivalent to an increase in resolution), leading to the development of a long coherence length scale in simulations.
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U2 - 10.1088/1538-4357/462/1/l5
DO - 10.1088/1538-4357/462/1/l5
M3 - Article
AN - SCOPUS:3943061373
SN - 0004-637X
VL - 462
SP - L5-L8
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1 PART II
ER -