Measurements of the cosmological density parameter (Ω) using techniques that exploit the gravity-induced motions of galaxies yield, in linear perturbation theory, the degenerate parameter combination β = Ω0.6/b, where the linear bias parameter b is the ratio of the fluctuation amplitudes of the galaxy and mass distributions. However, the relation between the mass and the galaxy density fields d...

We show that if a sample of galaxy clusters is complete above some mass threshold, then hierarchical clustering theories for structure formation predict its autocorrelation function to be determined purely by the cluster abundance and by the spectrum of linear density fluctuations. Thus if the shape of the initial fluctuation spectrum is known, its amplitude σ8 can be estimated directly from th...

Two little explored aspects of Compton scattering of the CMB in clusters are discussed: The statistical properties of the Sunyaev-Zeldovich (S-Z) effect in the context of a non-Gaussian density fluctuation field, and the polarization patterns in a hydrodynamcially-simulated cluster. We have calculated and compared the power spectrum and cluster number counts predicted within the framework of tw...

By averaging the basic equations on microscale. expressions are derived for the effective added mass density and the kinetic energy density of a mixture of liquid and gas bubbles. Due to hydrodynamic interaction between the bubbles there appears to be a difference between the effective added mass density and the mass coefficient of the kinetic energy density due to relative motion of the phases...

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Systems are more and more expected to work in dynamic environment, to deal with fluctuation of their characteristics and to guaranty functional and nonfunctional requirements. Systems should also keep compliant with the contracted quality of service. Moreover, when necessary, services and aspects should be added or removed on line. In this paper, we overview major approaches to deploy, reconfig...