Magnetic field transport in turbulent compressible convection (Chair: DJ Galloway)
Seminar Room 1, Newton Institute
Magnetic field transport is essential to certain elements of the solar dynamo scenario. It is crucial (a) to move poloidal field from the convection zone to the tachocline relatively quickly, and (b) to transport the magnetic structures created in the tachocline through the convection zone towards the solar surface, for the current dynamo paradigm to work. Here, we examine the competition between magnetic buoyancy and magnetic pumping mechanisms in such situations via high resolution numerical simulations of turbulent compressible penetrative magnetoconvection.