Abstract
The large-scale morphology of the high-density baryonic material in the universe, consisting of “clusters” in the form of pancakes, filaments, and nodes is obtained when matter streams away from a distribution of low-density expansion centres (“nuclei”) and collects in the interstices of a close packing of spheres.
This naturally leads to a partitioning of space generated by a process known as Voronoi tessellation. We have studied the statistical properties of specific instances of these tessellations, which we call Voronoi foams, for several model distributions of expansion centres. We derive the statistical properties of the regions where baryonic matter accumulates, and of the voids between the galaxies. These can be compared with observations, leading to indirect constraints on the initial spectrum of the density perturbations that produced the matter distribution we observe today.
The appearance of a Voronoi foam closely resembles the mass distribution found in numerical hydrodynamic experiments, and the bubble structure observed in the galaxy distribution.
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Icke, V. (1988). Voronoi foam as a model of the medium-scale universe. In: Seitter, W.C., Duerbeck, H.W., Tacke, M. (eds) Large-Scale Structures in the Universe Observational and Analytical Methods. Lecture Notes in Physics, vol 310. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-50135-5_78
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DOI: https://doi.org/10.1007/3-540-50135-5_78
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