Isotherms clustering in cosmic microwave background

Abstract

Since the strong clustering of luminous matter in the observable universe is a consequence of an initial non-uniformity of the baryon-photon fluid in the last scattering surface, an investigation of clustering of the isotherms in the cosmic microwave background has been performed. The isotherms clustering has been related to the baryon-photon fluid dynamics and the Taylor-microscale Reynolds number of this motion is estimated to be $10^2$. 3-year WMAP cosmic microwave background map has been used in this investigation.

References in corpus (13)

• A high resolution foreground cleaned CMB map from WMAP
• The inverse cascade and nonlinear alpha-effect in simulations of isotropic helical hydromagnetic turbulence
• Evidence of vorticity and shear at large angular scales in the WMAP data: a violation of cosmological isotropy?
• Scale-invariance of galaxy clustering
• Magnetohydrodynamics in the Early Universe and the Damping of Non-linear Alfven Waves
• Evolving turbulence and magnetic fields in galaxy clusters
• Magnetic Helicity Conservation and Astrophysical Dynamos
• Microwave Background Anisotropies from Alfven waves
• Does Fully-Developed Turbulence Exist? Reynolds Number Independence versus Asymptotic Covariance
• Generation of Cosmic Magnetic Fields and Gravitational Waves at Neutrino Decoupling
• Nonlinear Magnetic Diffusion and Magnetic Helicity Transport in Galactic Dynamos
• "Intermittency" in Hydrodynamic Turbulence as Intermediate Asymptotic to Kolmogorov41 Scaling
• Multiscaling of galactic cosmic ray flux

Cited by in corpus (10)

• The Origin of Life from Primordial Planets
• Long range correlation in cosmic microwave background radiation
• Gravitational hydrodynamics of large scale structure formation
• Evolution of proto-galaxy-clusters to their present form: theory and observations
• Decoupling and coherent plasma oscillations around last scattering
• Turbulence and turbulent mixing in natural fluids
• Evolution of proto-galaxy-clusters to their present form: theory and observations
• Turbulent formation of protogalaxies at the end of the plasma epoch: theory and observations
• Turbulent formation of protogalaxies at the plasma to gas transition
• Planets and Dark Energy