Modeling large-scale motions

It is not clear how improvements can be made without real progress on the difficult fundamental problems of diffusion in media with obstacles and cooperation of large-scale motions between interpenetrating chains which do not violate chain connectivity. The DeGennes reptation model (225) makes a significant contribution to the first problem, although in an admittedly simplified system. Rigorous calculations or computer simulations on well-defined models which relate to the second problem would be extremely valuable, even if the models themselves were not completely faithful representations of the assumed physical situation. It is not obvious how even to pose solvable problems, simplified or not, which relate to interchain cooperation. 

The filtered model equations are solved numerically for v(r,f), which provides a 3D and time dependent approximation to the large scale motions in one realization of the turbulent flow. 

Statistical models, in which the variables depend only on geographical latitude and time. In these models large scale atmospheric motions are taken into account statistically. 

T-H-M-C processes are significantly affected by subsurface heterogeneity, which results in scale-dependence of the related parameters. To handle this scale-dependent behavior, we need to characterize this heterogeneity and consider its effects at different scales. In this study, we demonstrate that the measured permeability data from Sellafield site, UK, are very well described by fractional Levy motion (fLm), a stochastic fractal. This finding has important implications for modeling large-scale coupled processes in heterogeneous fractured rocks. 

Gas flow in flow field can be described by Navi-er-Stokes equations, and then close equations by revised turbulent fluctuation RNG k-e two-way model, dealing with wall flow by wall function method (Wang et al. 2004). The model reflect the impact of small-scale through viscosity which is got after large-scale motion and amendments, remove small-scale movement systematically from... 

From radial velocities, together with a model of galactic rotation, one estimates "kinematic" distances (III.l). The line widths and shapes yield information on large-scale motions, turbulence and local electron densities. (II1.3). 

Dynamical models (e.g. [4, 5]) have been constructed to study the formation of these phases and their interplay. The whole pattern is dynamical, with supemovae explosions and stellar winds from massive stars creating bubbles of hot gas expanding through the diffuse medium, accompanied by large scale motions and shock waves. 

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