scholarly journals Computational Cosmology: From the Early Universe to the Large Scale Structure

2001 ◽  
Vol 4 (1) ◽  
Author(s):  
Peter Anninos
Keyword(s):  
Early Universe ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure

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.

EFFECTS OF PRIMORDIAL MAGNETIC FIELD ON EARLY UNIVERSE

2008 ◽  
Vol 23 (17n20) ◽  
pp. 1695-1706 ◽  
Author(s):  
DAI G. YAMAZAKI ◽  
KIYOTOMO ICHIKI ◽  
KAJINO TOSHITAKA ◽  
GRANT J. MATHEWS
Keyword(s):  
Magnetic Field ◽  
Power Spectrum ◽  
Cosmic Microwave Background ◽  
Early Universe ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Microwave Background ◽  
Primordial Magnetic Field

The existence of a primordial magnetic field (PMF) would affect both the temperature and polarization anisotropies of the cosmic microwave background (CMB) and the formation of the large scale structure(LSS). It also provides a plausible explanation for the disparity between observations and theoretical fits to the CMB power spectrum and the LSS. Here we report on calculations of not only the numerical power spectrum of the PMF, but also the correlations between the PMF power spectrum and the primary curvature perturbations.

scholarly journals Measuringαin the early universe: CMB temperature, large-scale structure, and Fisher matrix analysis

2002 ◽  
Vol 66 (2) ◽  
Author(s):  
C. J. A. P. Martins ◽  
A. Melchiorri ◽  
R. Trotta ◽  
R. Bean ◽  
G. Rocha ◽  
...  
Keyword(s):  
Early Universe ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Matrix Analysis ◽  
Fisher Matrix ◽  
Cmb Temperature

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.

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