A Lagrangian Particle‐based Formulation for Coupled Simulation of Fracture and Diffusion in Thin Membranes

2021 ◽  
Vol 40 (7) ◽  
pp. 97-108
Author(s):  
Chengguizi Han ◽  
Tao Xue ◽  
Mridul Aanjaneya
Keyword(s):  
Coupled Simulation ◽  
Lagrangian Particle ◽  
Thin Membranes ◽  
And Diffusion

scholarly journals Simulação da dispersão de poluentes na camada limite planetária utilizando um sistema de modelos

2000 ◽  
pp. 09 ◽  
Author(s):  
Jonas C. Carvalho ◽  
Gervásio Annes Degrazia ◽  
Domenico Anfossi ◽  
Silvia Trini Castelli
Keyword(s):  
Particle Model ◽  
Contaminant Plume ◽  
Lagrangian Particle ◽  
Temporal And Spatial Distribution ◽  
General Behaviour ◽  
Meteorological Model ◽  
Transport And Diffusion ◽  
Rhine Valley ◽  
Temporal And Spatial ◽  
And Diffusion

The meteorological model RAMS and the Lagrangian particle model SPRAY are coupled to simulate the transport and diffusion of tracer released during the project TRACT, realized in the Rhine valley, Central Europe. The simulation results generated by the model system are evaluated against observational data measured in the TRACT experiments. Analysis of the results and the application of statistical indices show that the considered models reproduce well the general behaviour of the contaminant plume, the temporal and spatial distribution of the concentration and the location of the concentration maxima.

Meridional Circulation, Turbulence, and Diffusion Processes in Stars

1976 ◽  
Vol 32 ◽  
pp. 109-116 ◽  
Author(s):  
S. Vauclair
Keyword(s):  
Convection Zone ◽  
Diffusion Processes ◽  
Meridional Circulation ◽  
Diffusion Time ◽  
Work In Progress ◽  
First Results ◽  
Stellar Envelopes ◽  
And Diffusion ◽  
Turbulence And Diffusion ◽  
Hr Diagram

This paper gives the first results of a work in progress, in collaboration with G. Michaud and G. Vauclair. It is a first attempt to compute the effects of meridional circulation and turbulence on diffusion processes in stellar envelopes. Computations have been made for a 2 Mʘstar, which lies in the Am - δ Scuti region of the HR diagram.Let us recall that in Am stars diffusion cannot occur between the two outer convection zones, contrary to what was assumed by Watson (1970, 1971) and Smith (1971), since they are linked by overshooting (Latour, 1972; Toomre et al., 1975). But diffusion may occur at the bottom of the second convection zone. According to Vauclair et al. (1974), the second convection zone, due to He II ionization, disappears after a time equal to the helium diffusion time, and then diffusion may happen at the bottom of the first convection zone, so that the arguments by Watson and Smith are preserved.

Ordering and diffusion in II-VI/III-VI alloys with structural vacancies

1997 ◽  
Vol 101-103 (1-2) ◽  
pp. 479-487
Author(s):  
H v. Wensierski
Keyword(s):  
And Diffusion
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