3D Global Modeling of the Solar Dynamo

We are attempting to use 3D global MHD models to accurately reproduce the magnetic dynamo and other patterns of solar activity. Our work is focused on modeling the entire solar convection zone so that we can try to reproduce the interconnected effects that generate the solar cycle. Using data from standard reference models, such as the model S [4], we map the ambient state for a polytropic ideal gas and solve for its advection to model the propagation of turbulent convective transport and magnetic induction throughout the region. We use new approaches to these models to better understand the impact that different parameters can have on an evolving system. We model 3 different resolutions with the following grid points: (512 {\phi}, 256 {\theta}, 256 R), (256 {\phi}, 128 {\theta}, 128 R) and (128 {\phi}, 64 {\theta}, 64 R), as well as varying models of convection. The 2 higher resolution models express an implicit viscosity that is just too unrealistic to take away any significant results, however the changes in convection profiles in the low resolution models show how minor changes in convection can change the axisymmetric pattern of the dynamo cycle.