Smoothed particles hydrodynamics numerical simulations of droplets walking on viscous vibrating liquid

Explicit dynamics “SPH – Finite Element” coupling using the Arlequin method

European Journal of Computational Mechanics ◽

10.13052/remn.17.737-748 ◽

2008 ◽

pp. 737-748

Author(s):

Yann Chuzel-Marmot ◽

Alain Combescure ◽

Roland Ortiz

Keyword(s):

Experimental Study ◽

Finite Element ◽

Finite Elements ◽

Numerical Simulations ◽

Concrete Slab ◽

Explicit Dynamics ◽

Arlequin Method ◽

Smoothed Particles Hydrodynamics ◽

Projectile Impacts

The Arlequin method gives a simple and effective framework to glue models using various formulations. It is extended here in explicit dynamics and used in order to link a zone showing ruptures by fragmentation meshed with Smoothed Particles Hydrodynamics (SPH) and a larger second undamaged one meshed with finite elements (FEM). This paper gives some details on the method implemented in the EUROPLEXUS code, its validation on simple benchmarks and a confrontation between numerical simulations and results of an experimental study of concrete slab resistance to projectile impacts.

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Direct Numerical Simulations of Gas–Liquid Multiphase Flows

10.1017/cbo9780511975264 ◽

2001 ◽

Cited By ~ 151

Author(s):

Grétar Tryggvason ◽

Ruben Scardovelli ◽

Stéphane Zaleski

Keyword(s):

Numerical Simulations ◽

Multiphase Flows ◽

Direct Numerical Simulations

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Saturation mechanism and generated viscosity in gravito-turbulent accretion disks

Astronomy and Astrophysics ◽

10.1051/0004-6361/202038023 ◽

2020 ◽

Vol 640 ◽

pp. A53

Author(s):

L. Löhnert ◽

S. Krätschmer ◽

A. G. Peeters

Keyword(s):

Growth Rate ◽

Numerical Simulations ◽

Accretion Disks ◽

Gravitational Instability ◽

Turbulent Viscosity ◽

Radial Distance ◽

Maximum Growth ◽

Wave Number ◽

Radiative Cooling ◽

Mixing Length

Here, we address the turbulent dynamics of the gravitational instability in accretion disks, retaining both radiative cooling and irradiation. Due to radiative cooling, the disk is unstable for all values of the Toomre parameter, and an accurate estimate of the maximum growth rate is derived analytically. A detailed study of the turbulent spectra shows a rapid decay with an azimuthal wave number stronger than ky−3, whereas the spectrum is more broad in the radial direction and shows a scaling in the range kx−3 to kx−2. The radial component of the radial velocity profile consists of a superposition of shocks of different heights, and is similar to that found in Burgers’ turbulence. Assuming saturation occurs through nonlinear wave steepening leading to shock formation, we developed a mixing-length model in which the typical length scale is related to the average radial distance between shocks. Furthermore, since the numerical simulations show that linear drive is necessary in order to sustain turbulence, we used the growth rate of the most unstable mode to estimate the typical timescale. The mixing-length model that was obtained agrees well with numerical simulations. The model gives an analytic expression for the turbulent viscosity as a function of the Toomre parameter and cooling time. It predicts that relevant values of α = 10−3 can be obtained in disks that have a Toomre parameter as high as Q ≈ 10.

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