Large-Scale Structure of the Universe in Unstable Dark Matter Models

1988 ◽  
pp. 293-300
Author(s):  
A. G. Doroshkevich ◽  
A. A. Klypin ◽  
M. U. Khlopov
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

scholarly journals Large-Scale Structure in the Universe: Spatial Distribution and Peculiar Velocities

1987 ◽  
Vol 124 ◽  
pp. 335-348
Author(s):  
Neta A. Bahcall
Keyword(s):  
Dark Matter ◽  
Spatial Distribution ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Clusters Of Galaxies ◽  
Large Scale Structures ◽  
Peculiar Velocities ◽  
Scale Structures ◽  
The Universe

The evidence for the existence of very large scale structures, ∼ 100h−1Mpc in size, as derived from the spatial distribution of clusters of galaxies is summarized. Detection of a ∼ 2000 kms−1 elongation in the redshift direction in the distribution of the clusters is also described. Possible causes of the effect are peculiar velocities of clusters on scales of 10–100h−1Mpc and geometrical elongation of superclusters. If the effect is entirely due to the peculiar velocities of clusters, then superclusters have masses of order 1016.5M⊙ and may contain a larger amount of dark matter than previously anticipated.

scholarly journals Large-Scale Structure of the Universe in Unstable Dark Matter Models

1988 ◽  
Vol 130 ◽  
pp. 293-300
Author(s):  
A.G. Doroshkevich ◽  
A.A. Klypin ◽  
M.U. Khlopov
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Large Scale ◽  
Numerical Models ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Microwave Background ◽  
Physical Background ◽  
The Mean ◽  
The Universe

Processes of the formation and the evolution of the large-scale structure are discussed in the framework of unstable dark matter models. Six numerical models are presented. The projected distribution of simulated galaxies on the sky, wedge diagrams, correlation functions and the mean linear scale of voids are presented. Physical background of the hypothesis of unstable particles and possible observational tests are discussed. The level of the microwave background fluctuations is estimated analytically. Special attention is given to late stage of supercluster evolution and galaxy formation.

scholarly journals Modelling the Large Scale Structure of the Universe after COBE

1995 ◽  
Vol 48 (6) ◽  
pp. 1083 ◽  
Author(s):  
PJ Quinn
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Cold Dark Matter ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Expanding Universe ◽  
Model Predictions ◽  
Perturbation Spectrum ◽  
The Universe

N-body models running on supercomputers have been widely used to explore the development of structure in the expanding Universe. Recent results from the COBE satellite have provided a global normalisation of these models which now allows detailed comparisons to be drawn between observations and model predictions. Some predictions of the cold dark matter primordial perturbation spectrum are now shown to be consistent with surveys of galaxy redshifts.

The large-scale structure of the universe in skewed cold dark matter models

1992 ◽  
Vol 1 (1) ◽  
pp. 99-112 ◽  
Author(s):  
A. Messina ◽  
F. Lucchin ◽  
S. Matarrese ◽  
L. Moscardini
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Cold Dark Matter ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

COSMIC STRINGS, HOT DARK MATTER AND THE LARGE-SCALE STRUCTURE OF THE UNIVERSE

1990 ◽  
Vol 05 (09) ◽  
pp. 1633-1651 ◽  
Author(s):  
ROBERT H. BRANDENBERGER ◽  
LEANDROS PERIVOLAROPOULOS ◽  
ALBERT STEBBINS
Keyword(s):  
Dark Matter ◽  
Galaxy Formation ◽  
Large Scale ◽  
Cosmic Strings ◽  
Unit Length ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Rotation Curves ◽  
The Universe

A review of recent results on large-scale structure and galaxy formation in a model with hot dark matter and cosmic strings is given. With cosmic strings seeding perturbations, many of the arguments against hot dark matter disappear. It is shown that spherical accretion about loops leads to dark matter haloes with flat velocity rotation curves. Velocity perturbations due to wakes behind long, moving strings lead to a network of planar overdensities with a distinguished scale of slightly less than 40×40 Mpc2. If the mass per unit length μ exceeds a certain bound, then the wakes become nonlinear by the present time. In this case, their thickness can be calculated.

scholarly journals A Scalar Field Dark Matter Model and Its Role in the Large-Scale Structure Formation in the Universe

2012 ◽  
Vol 2012 ◽  
pp. 1-13 ◽  
Author(s):  
Mario A. Rodríguez-Meza
Keyword(s):  
Dark Matter ◽  
Scalar Field ◽  
Structure Formation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Matter Model ◽  
The Universe ◽  
Dark Matter Model ◽  
Large Scale Structure Formation

We present a model of dark matter based on scalar-tensor theory of gravity. With this scalar field dark matter model we study the non-linear evolution of the large-scale structures in the universe. The equations that govern the evolution of the scale factor of the universe are derived together with the appropriate Newtonian equations to follow the nonlinear evolution of the structures. Results are given in terms of the power spectrum that gives quantitative information on the large-scale structure formation. The initial conditions we have used are consistent with the so-called concordance ΛCDM model.

scholarly journals Constraints on Dark Matter Density and Axion Mass from the Large-Scale Structure of Spacetime

1987 ◽  
Vol 117 ◽  
pp. 491-491
Author(s):  
P.S. Joshi ◽  
B. Datta
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Large Scale Structure ◽  
Maximum Density ◽  
Scale Structure ◽  
Axion Mass ◽  
Upper Limits ◽  
Age Of The Universe ◽  
Lower Limits ◽  
The Universe

On the basis of general properties of the large-scale structure of spacetime, we present new and general theoretical upper limits on the density of dark matter in the Universe, assuming a 90% content for the dark matter, and lower limits on the mass of the axion, assuming the dark matter to be made up of axions. These limits are derived in terms of the possible lower limits to the age of the Universe and the Hubble parameter. We find that for the age in the range (8–24) × 109yr, the maximum density of dark matter is in the range (1.25 × 10−28 −1.38 × 10−29) g cm−3 and the minimum value of axion mass in the ranges (0.36–2.39) × 10−5 eV and (1.44–9.51) × 10−5 eV.

Dark matter and the formation of large-scale structure in the Universe

1986 ◽  
Vol 119 (1) ◽  
pp. 247-248
Author(s):  
Lizhi Fang ◽  
Shouping Xiang ◽  
Shuxian Li ◽  
YaoQuan Chu ◽  
Xingfen Zhu
Keyword(s):  
Dark Matter ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe
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