Evolution of superclusters and supercluster cocoons in various cosmologies. (arXiv:2005.03480v2 [astro-ph.CO] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Einasto_J/0/1/0/all/0/1">J. Einasto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hutsi_G/0/1/0/all/0/1">G. Hütsi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suhhonenko_I/0/1/0/all/0/1">I. Suhhonenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liivamagi_L/0/1/0/all/0/1">L. J. Liivamägi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Einasto_M/0/1/0/all/0/1">M. Einasto</a>

We investigate the evolution of superclusters and supercluster cocoons

(basins of attraction), and the influence of cosmological parameters to the

evolution. We perform numerical simulations of the evolution of the cosmic web

for different cosmological models: the LCDM model with a conventional value of

the dark energy (DE) density, the open model OCDM with no DE, the standard SCDM

model with no DE, and the Hyper-DE HCDM model with an enhanced DE density

value. We find ensembles of superclusters of these models for five evolutionary

stages, corresponding to the present epoch z = 0, and to redshifts z = 1, 3,

10, 30. We use diameters of the largest superclusters and the number of

superclusters as percolation functions to describe properties of the ensemble

of superclusters in the cosmic web. We analyse the size and mass distribution

of superclusters in models and in real Sloan Digital Sky Survey (SDSS) based

samples. In all models numbers and volumes of supercluster cocoons are

independent on cosmological epochs. Supercluster masses increase with time, and

geometrical sizes in comoving coordinates decrease with time, for all models.

LCDM, OCDM and HCDM models have almost similar percolation parameters. This

suggests that the essential parameter, which defines the evolution of

superclusters, is the matter density. The DE density influences the growth of

the amplitude of density perturbations, and the growth of masses of

superclusters, albeit significantly less strongly. The HCDM model has the

largest speed of the growth of the amplitude of density fluctuations, and the

largest growth of supercluster masses during the evolution. Geometrical

diameters and numbers of HCDM superclusters at high threshold densities are

larger than for LCDM and OCDM superclusters. SCDM model has about two times

more superclusters than other models; SCDM superclusters have smaller diameters

and masses.

We investigate the evolution of superclusters and supercluster cocoons

(basins of attraction), and the influence of cosmological parameters to the

evolution. We perform numerical simulations of the evolution of the cosmic web

for different cosmological models: the LCDM model with a conventional value of

the dark energy (DE) density, the open model OCDM with no DE, the standard SCDM

model with no DE, and the Hyper-DE HCDM model with an enhanced DE density

value. We find ensembles of superclusters of these models for five evolutionary

stages, corresponding to the present epoch z = 0, and to redshifts z = 1, 3,

10, 30. We use diameters of the largest superclusters and the number of

superclusters as percolation functions to describe properties of the ensemble

of superclusters in the cosmic web. We analyse the size and mass distribution

of superclusters in models and in real Sloan Digital Sky Survey (SDSS) based

samples. In all models numbers and volumes of supercluster cocoons are

independent on cosmological epochs. Supercluster masses increase with time, and

geometrical sizes in comoving coordinates decrease with time, for all models.

LCDM, OCDM and HCDM models have almost similar percolation parameters. This

suggests that the essential parameter, which defines the evolution of

superclusters, is the matter density. The DE density influences the growth of

the amplitude of density perturbations, and the growth of masses of

superclusters, albeit significantly less strongly. The HCDM model has the

largest speed of the growth of the amplitude of density fluctuations, and the

largest growth of supercluster masses during the evolution. Geometrical

diameters and numbers of HCDM superclusters at high threshold densities are

larger than for LCDM and OCDM superclusters. SCDM model has about two times

more superclusters than other models; SCDM superclusters have smaller diameters

and masses.

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