Solar magnetism simulation

Solar magnetism simulation

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Credit: NASA/Ames (Irina Kitiashvili, Stanford University; Tim Sandstrom)/SCIENCE PHOTO LIBRARY

Caption: Solar magnetism simulation. Supercomputer simulation of magnetic structures formed by a turbulent dynamo on the Sun. In the Sun, highly turbulent hot plasma flows stretch, twist, and fold magnetic field lines, resulting in magnetoconvection. Here, magnetic field lines form a 'carpet' of magnetic loops at a temperature of 6400 degrees Kelvin. This simulation is one of several Large-Eddy Simulations produced with the parallel 3D radiative magnetohydrodynamic code SolarBox, using NASA's Pleiades supercomputer. The simulation was featured at the SC13 supercomputing conference in November 2013.

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Keywords: 2013, 21st century, 3d, astrophysical, astrophysics, graphic, heliophysics, illustration, large-eddy simulation, lhs, magnetic field lines, magnetic loop, magnetohydrodynamic, magnetohydrodynamics, mhd, model, nasa advanced supercomputing, no-one, nobody, parallel, physics, pleiades supercomputer, radiative, sc13, simulation, solar, solar magnetism, solar magnetism simulation, solar physics, solar structure, solar system, space, sun, supercomputer, supercomputing conference, surface, turbulent dynamo

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