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Views of solar convection and entropy
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Views of solar convection and entropy.

May 26, 2010
Views of solar convection and entropy. Robert Stein, a physics and astronomy professor at Michigan State University, and Aake Nordlund of Copenhagen University Observatory in Denmark used the National Computational Science Alliance's SGI Origin2000 supercomputer at the National Center for Supercomputing Applications (NCSA) to create massive models of portions of the sun and to simulate the processes behind the sun's smaller-scale features. One of their projects covered a swath of the sun 18,000-km square, and extending from the surface to 9,000 km in depth. [Image 1 of 4 related images. See Image 2.]

More about this Image Using the models, the team focused on understanding convection and magnetic flux near the solar surface. Rather than create the simulation through a variety of modeling applications, the team uses a single, integrated code that's based on the laws of conservation of mass, momentum and energy, as well as the forces of pressure, gravity and the magnetic field. Solving the equations that represent these laws and forces allow the researchers to see the essential physics at work, the radiative cooling at the surface that drives convection, and the turbulent motions that generate small-scale, magnetic fields and shuffle them around, for example.

On 4 to 6 Origin2000 processors, it takes about one day to simulate 30 seconds of time on the sun. Eventually, they hope to simulate about one day on the sun.

Using the team's newest simulations, they hope to learn how much small-scale magnetic flux is generated by convection, how larger-scale structures are related to granulation, and how to calibrate sound waves to observe phenomena near the solar surface.

This work was supported by grants from the National Science Foundation (grants AST 95-21785 and AST 98-19799), NASA and the Danish Research Council.