Abstract
The approach to the problem of large-scale structure of the Universe is considered where an initial linear peculiar gravitational potential \(\varphi (\vec x)\) plays the crucial role. The random field ϕ contains all information about the particular cosmological model. 1 Voids form around high peaks of ϕ, the large-scale streaming velocities of galaxies 1 are governed by ‘hills’ and ‘valleys’ of ϕ. The mechanisms of the generation of non-standard 1 (non-flat and non-Gaussian) initial perturbations at the inflationary stage are briefly discussed in terms of ϕ. 1
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Kofman, L. (1989). Structure of the Universe via gravitational potential. In: Flin, P., Duerbeck, H.W. (eds) Morphological Cosmology. Lecture Notes in Physics, vol 332. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-51223-3_136
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DOI: https://doi.org/10.1007/3-540-51223-3_136
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