The investigators seek to understand the large-scale dynamics of solar flux tubes that lead to the morphology and evolution of active regions. Flux tube buoyancy is influenced by the rotation rate of the Sun (or star). Shear flows and shear rotation can enhance the accumulation of magnetic energy and thus its release. The orientation of currents in the flux tubes, as well as helicity of the magnetic field is also important in emergence of flux and interaction of flux tubes. The main effort is to employ analytical methods and numerical simulations to illuminate the effects of differential solar rotation on flux emergence and flux tube reconnection. Computational and theoretic results will be corroborated by observations from the Yokoh and SOHO spacecraft.
