beta-Plane Turbulence

My 2D Hydrodynamic GPU code is over an order of magnitude faster than CPU codes (its source is available on GitHub). It is wasteful if I do not apply it to study some (astro-) physical problems. It turns out that, by introducing a simple \beta-term, the modified vorticity equation

    \[ \frac{\partial\omega}{\partial t} = J(\phi, \omega) + \nu \nabla^2\omega - \mu\omega - \beta u_y, \]

can take into account Coriolis force. The above equation is now a local (and, of course, two-dimensional) representation of the atmosphere on planets. This so called \beta-plane approximation is used to study zonal jets of Jupiter’s atmosphere.

Jupiter by Cassini-Huygens

So I started playing around with the new equation. It will take me a while to find out what are the important questions to address. Nevertheless, the following movie shows a subdomain of a two-dimensional, incompressible hydrodynamic test-run in the \beta-plane. The color, just like my previous movies, represents vorticity.

I would like to thank PDC for providing the Zorn cluster, which makes the development possible. The Zorn cluster is named after a painter Anders Zorn because it has GPUs. The code is now available for download on GitHub.


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