Solar convection and magnetic fields

Thermal convection is the most significant driver of time-dependent patterns of motion within the Sun. Observations of magnetic and convection phenomena in the Sun, together with an understanding of the basic physical processes involved, provide a basis for large numerical simulations. Models of solar convection produced in this way and using considerable computer power can investigate such problems as the role of stratification within the Sun, in two or three dimensions. The models are now sufficiently complex to produce results that can be compared with observations, in some cases. In future this technique offers the chance to replicate surface solar phenomena such as sunspots, while uncovering the complex magnetoconvection beneath.