FLASH is an adaptive mesh hydrodynamics code for modeling astrophysical thermonuclear flashes. The FLASH code was developed to study the problems of nuclear flashes on the surfaces of neutron stars and white dwarfs, as well as in the interior of white dwarfs. The FLASH code solves the fully compressible, reactive hydrodynamic equations and allows for the use of adaptive mesh refinement. It also contains state-of-the-art modules for the equations of state and thermonuclear reaction networks.

More information can be found at: http://flash.uchicago.edu/website/home/

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