This is a depiction of a magnetic binary star, such as an RS Canum Venaticorum (RS CVn) system. A typical RS CVn binary consists of two stars in a tight gravitational bind, only a few stellar radii apart, the orbital period usually in the range several hours to a few days. One star is always an orange subgiant; the other is somewhat like the Sun, yellow, or occasionally a somewhat hotter yellow-white. The hallmarks of these stars are gigantic magnetic fields, which I show here giving rise to flaring and gargantuan starspots.