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Browsing by Author "Penders, Sam"

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    Magnetic Filament Formation in the Intracluster Medium
    (2019) Penders, Sam;
    Results from a high–resolution, turbulent, magnetohydrodynamics simulatation, with conditions that mimic those of a galaxy cluster plasma, are analyzed to determine the source of magnetic field filamentation. Although this simulation does not explicitly model resistive contributions to magnetic field growth, it was determined that numerical energy dissipation is approximately equal in magnitude and opposite in sign to magnetic energy growth predicted by ideal magnetohydrodynamics. Resistive energy dissipation is therefore essential to magnetic field filamentation.
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    Visualizations from a Magnetohydrodynamic Turbulence model of the Intracluster Medium
    (2019-05) Penders, Sam; Jones, Thomas W; Porter, David H; dhp@umn.edu; David Porter
    The intracluster medium (ICM) is a tenuous plasma between galaxies. Long parallel strands of strong magnetic fields are seen in the ICM. These movies show the development of turbulence and the growth of magnetic fields in a numerical model of magnetohydrodynamic (MHD) turbulence. The computational model was ideal Isothermal MHD. The flow was computed in a periodic box on a uniform 1024 x 1024 x 1024 mesh. The velocity field was continually stirred with random long wavelength sine wave accelerations, which mimics the effect of changing gravitational field due to galaxies moving in the cluster. The B-field was initially uniform and very weak, with the magnetic pressure one million times weaker than gas pressure. Over the span of the simulation, the magnetic pressure increased to about 5% of the gas pressure and was strong enough to strongly influence the flow. The numerical simulation was run on the Minnesota Supercomputer Institute’s Mesabi cluster: using 22 compute nodes (two Intel Haswell 12-core Processors per node) for 44 hours.