Explore chapters and articles related to this topic
The Earth Through Time
Published in Aurèle Parriaux, Geology, 2018
The formation of our solar system is probably the result of the accretion of matter. About 4.6 Ga ago, a part of our galaxy underwent gravitational accretion that gave rise to our solar system. A cloud of particles condensed as it revolved around an axis passing through the point of maximum concentration, which became our sun.
The Earth in Time
Published in Aurèle Parriaux, Geology, 2018
The formation of our solar system is probably the result of the accretion of matter. About 4.6 Ga ago, a part of our galaxy underwent gravitational accretion that gave rise to our solar system. A cloud of particles condensed as it revolved around an axis passing through the point of maximum concentration, which became our Sun.
“Simulation of medical goggles to stop airborne transmission of viruses: computational fluid dynamics in ergonomics”
Published in Ergonomics, 2023
Wenxiu Yang, Tingshu Chen, Haining Wang, Renke He
To understand the distribution and density of particle deposition, the accretion rate and contour were selected as the metrics. The accretion rate is defined as the mass of particles per unit area deposited in an area, indicating the mass of droplets per unit area deposited on the model surface. In Ansys Fluent, the accretion rate equation in the DPM is defined as: where is the number of particles, is the area of the cell surface at the wall, and is the mass flow rate of the particles, and the accretion rate is expressed in units of kg/m2.
Introduction
Published in Geophysical & Astrophysical Fluid Dynamics, 2021
Benjamin Favier, Michael Le Bars, Stéphane Le Dizès, Patrice Le Gal, Patrice Meunier
In the work of G. Meletti et al., numerical simulations are complemented by laboratory experiments on the Strato-Rotational Instability (SRI) making the rotating shear flow unstable in regions where – without stratification – it would be stable. As proposed in their article, this characteristic renders SRI a relevant phenomenon in planetary and astrophysical applications, particularly in the magnetically dead zones of accretion disks.