We will learn:

How magnetic fields build up and decay in the Sun. How and where electric currents are generated by the magnetic field. How to detect magnetic fields before they emerge. How the Sun's internal structure and surface change during the 11-year cycle. Whether solar convection changes during the cycle. How the solar diameter varies during the cycle. How total solar irradiance changes over the cycle. The reasons for spectral irradiance changes.

How magnetic energy is converted into radiation, heat, and mass motion. How the corona is heated. What drives the solar wind. Where the energy for coronal mass ejections is stored. What triggers coronal mass ejections. Where explosive flare energy release begins. What processes accelerate particles. How accelerated particles and plasmas interact. What properties of solar eruptions forecast important consequences for Earth.