This talk will address the origin of the 11-year (quasi-) periodicity of the sunspot cycle by tying it to the significant temporal overlap of activity bands belonging to the 22-year magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints, and the prevalent magnetic scale on which they form, we are able to observationally demonstrate the entirety of the 22-year magnetic activity cycle. The phases of the sunspot cycle occur as landmarks in the interaction and evolution of the overlapping activity bands in each hemisphere. The work presented establishes significant observational constraints for models of the origins of solar magnetic activity and will, as a result, improve our understanding of the structure of the heliosphere and the modulation of our star’s radiative and particulate output. If time permits, we will explore some of the short-term variability in the system that are relevant to space weather.