Solar Torsional Oscillation in the Presence of Convection
The torsional oscillation is a perturbation to the differential rotation in the convection zone of the sun that is spatially correlated with sunspot activity. Previous work has examined conditions necessary for the torsional oscillation to propagate through the convection zone using mean-field models with parameterized convection. This project examines the propagation behavior using an axisymmetric magnetohydrodynamic model utilizing explicit convection. Specifically, stationary perturbations will be generated at three different latitudes to provide a direct comparison to previous work. Further, perturbations traveling from a latitude of 45° both poleward and equatorward will be used to assess the effect of motion on the propagation. The resources at MSI are necessary because the simulations are very large. The grid contains 1,500 nodes, and three variables must be computed at each node. Each simulation will last for several million time steps. The code requires the use of an Intel Fortran compiler and MPI.
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