Speaker
Description
The solar photosphere is shaped by the interplay between convection and magnetic fields, producing a rich variety of structures in active regions. While granulation represents the fundamental convective pattern of the quiet Sun, magnetic field in active regions gives rise to distinct magneto-convective regimes, each defined by a different balance between plasma motions and magnetic forces. Observations and MHD simulations suggest that these regimes are organized around key magnetic field thresholds, which govern the morphology, brightness, and dynamics of features such as umbrae and penumbrae. However, our current understanding relies largely on analyses of observations with limited spatial and temporal resolution, restricting us to statistical descriptions of stable structures and obscuring the dynamic transitions between observed regimes. These transient processes—where convection rapidly reorganizes under evolving magnetic conditions—are fundamental to understand evolution of structures in active regions and the fine-scale interplay between magnetic and kinetic forces. In this talk, I will highlight some of the Sunrise III datasets offering a promising opportunity to understand more details about magneto-convective regimes.