scholarly journals Large Scale Structure of the Universe: Theoretical Problems

1990 ◽  
Vol 43 (2) ◽  
pp. 159
Author(s):  
E Saar
Keyword(s):  
Early Universe ◽  
Present Status ◽  
Large Scale ◽  
Large Scale Structure ◽  
Short Review ◽  
Fractal Model ◽  
Scale Structure ◽  
The Subject ◽  
The Universe

Implications of the observed large scale structure on the physics of the early universe are described. A short review of Soviet work on the subject is given, and the present status of the fractal model of the large scale structure is discussed.

scholarly journals The Fractal Turbulence and the Origin of Large Scale Structure

1988 ◽  
Vol 130 ◽  
pp. 553-553
Author(s):  
Y.-Z. Liu ◽  
Z.-G. Deng
Keyword(s):  
Early Universe ◽  
Large Scale ◽  
Hubble Constant ◽  
Large Scale Structure ◽  
Thomson Scattering ◽  
Scale Structure ◽  
Scale Free ◽  
Density Perturbations ◽  
Reynold’S Number ◽  
The Universe

We have suggested a scenario of fractal turbulence which might explain the origin of galaxies and the observed large scale structure of the universe (Liu and Deng, 1987). Under the condition of the early universe, the cosmic fluid can be regarded as incompressible. If we assume that the density perturbations in the early universe are adiabatic and have the scale-free Zeldovich spectrum, we may obtain the spectrum of the velocity perturbations. Perturbations with scales less than horizon will undergo dissipative process by Thomson scattering. So, the cosmic fluid can be considered as a viscous fluid (Peebles, 1971). We can find the largest and smallest scale of the perturbations in the cosmic fluid by taking account of the Reynold's number on given scale and the scale of horizon. Using the present values of Hubble constant and the mean density of matter, we have found that on the scale of horizon the Reynold's number is just the order of 102. This result shows that perturbations with scale a little smaller than horizon may produce Karman vortices before recombination and the vortices might form fractal turbulence due to Thomson drag.

LARGE SCALE STRUCTURE OF THE UNIVERSE — A POWERFUL PROBE FOR FUNDAMENTAL PHYSICS

2012 ◽  
Vol 12 ◽  
pp. 100-109 ◽  
Author(s):  
JAAN EINASTO
Keyword(s):  
Early Universe ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Fundamental Physics ◽  
Sky Surveys ◽  
Physical Conditions ◽  
Physical Experiments ◽  
The Universe

An overview is given on properties of the Large Scale Structure (LSS) using recent sky surveys (SDSS Main sample). LSS evolves very slowly, thus it contains imprints of physical conditions in the early Universe, as well as processes during its evolution. Present physical experiments are still unable to reproduce conditions in the very early Universe, thus the study of the properties of the LSS yields valuable information for fundamental physics.

scholarly journals Baryogenesis in the Inflationary Universe

1987 ◽  
Vol 117 ◽  
pp. 492-492
Author(s):  
Hideo Kodama ◽  
Katsuhiko Sato ◽  
Nobuaki Sato
Keyword(s):  
Standard Model ◽  
Early Universe ◽  
Large Scale ◽  
Large Scale Structure ◽  
Baryon Asymmetry ◽  
Scale Structure ◽  
Inflationary Universe ◽  
Universe Model ◽  
Number Density ◽  
The Universe

As is known well, the inflationary universe model resolves most of the fundamental problems concerning the large scale structure of the universe and is now becoming a standard model for the early universe. However, there is one important problem yet to be made clear. In this model the number density of particles effectively goes to zero during the inflation and everything is created after the universe is heated up again at the end of inflation. Since the reheating temperature is much lower than the GUT temperature in general, however, it is not clear whether the observed baryon asymmetry is generated in this process.

scholarly journals The internal structure of protoclusters and the formation of galaxies

1978 ◽  
Vol 79 ◽  
pp. 423-425 ◽  
Author(s):  
A. G. Doroshkevich ◽  
E. M. Saar ◽  
S. F. Shandarin
Keyword(s):  
Internal Structure ◽  
Large Scale ◽  
Large Scale Structure ◽  
Short Review ◽  
Scale Structure ◽  
Clusters Of Galaxies ◽  
General Picture ◽  
Adiabatic Theory ◽  
The Universe

We give a short review of the general picture and main features of the formation of galaxies and clusters of galaxies on the basis of the adiabatic theory. Detailed discussions of these questions are published in references 1–6. Some related problems of the formation and development of large scale structure in the Universe according to the same theory are considered in Zeldovich's report.

scholarly journals Formation of the large-scale structure of the Universe

2011 ◽  
Vol 54 (10) ◽  
pp. 983-1005 ◽  
Author(s):  
Vladimir N Lukash ◽  
Elena V Mikheeva ◽  
A M Malinovsky
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

The Large‐Scale Structure of the Universe

Physics Today ◽  
1981 ◽  
Vol 34 (8) ◽  
pp. 62-63 ◽  
Author(s):  
P. J. E. Peebles ◽  
Simon D. M. White
Keyword(s):  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

scholarly journals The Theory of the Large Scale Structure of the Universe

1978 ◽  
Vol 79 ◽  
pp. 409-421 ◽  
Author(s):  
Ya B. Zeldovich
Keyword(s):  
Early Childhood ◽  
Sigmund Freud ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Other ◽  
Childhood Experiences ◽  
Other Hand ◽  
The Universe ◽  
Single Statement

The God-father of psychoanalysis Professor Sigmund Freud taught us that the behaviour of adults depends on their early childhood experiences. in the same spirit, the problem of cosmological analysis is to derive the observed present day situation and structure of the Universe from certain plausible assumptions about its early behaviour. Perhaps the most important single statement about the large scale structure is that there is no structure at all on the largest scale − 1000 Mpc and more. On this scale the Universe is rather uniform, structureless and isotropically expanding - just according to the simplified pictures of Einstein-Friedmann……. Humason, Hubble…. Robertson, Walker. On the other hand there is a lot of structure on the scale of 100 or 50 Mpc and less. There are clusters and superclusters of galaxies.

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