Thermohaline circulation and geostrophic planetary equation: physical, numerical and mathematical properties
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Publication:1826248
DOI10.5802/ambp.156zbMath1125.86304OpenAlexW2319124549MaRDI QIDQ1826248
Thierry Huck, Mamadou Sy, Bresch, Didier
Publication date: 5 August 2004
Published in: Annales Mathématiques Blaise Pascal (Search for Journal in Brave)
Full work available at URL: http://www.numdam.org/item?id=AMBP_2002__9_2_181_0
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Cites Work
- Solutions fortes et comportement asymptotique pour un modèle de convection naturelle en milieu poreux. (Strong solutions and asymptotic behaviour for a natural convection problem in porous media)
- Rotating fluid at high Rossby number driven by a surface stress: existence and convergence
- Convection in rotating porous media: The planetary geostrophic equations, used in geophysical fluid dynamics, revisited
- Computational design for long-term numerical integration of the equations of fluid motion: two-dimensional incompressible flow. Part I
- Coriolis effect on gravity-driven convection in a rotating porous layer heated from below
- Some mathematical properties of the planetary geostrophic equations for large-scale ocean circulation
- Global well‐posedness and finite‐dimensional global attractor for a 3‐D planetary geostrophic viscous model
- Regularity results for the stationary primitive equations of the atmosphere and the ocean
- Remarks on the planetary geostrophic model of gyre scale ocean circulation
- A fully implicit model of the three-dimensional thermohaline ocean circulation
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