Solar Active Regions: A Transition from Morphological Observations to Physical Modeling (Opening Keynote Address)

摘要

Although solar active regions can easily be identified from their sunspot groups, they keep some of the most challenging secrets of solar physics, regarding their subphotospheric origin, photospheric emergence, magnetic field structure, magnetic helicity, wave generation, propagation and dissipation, plasma heating and cooling, plasma flows, fractal geometry and intermittency, and magnetic instabilities leading to flares, CMEs, and coronal dimming. In this opening talk we review how morphological observations of active regions have gradually evolved into a more physics-based modeling approach over the last decades.