The two components of the solar activity cycle as a consequence of the shock transition model of the solar magnetic cycle

Abstract

Justification is given for comparing the consequences of the shock transition model of the solar magnetic cycle with important observed properties of the solar activity cycle without waiting for the basic postulates of the model to be mathematically established. Such a comparison shows that the creation and the evolution of the two topologically distant families of magnetic flux tubes and their different spatial distributions can account for the two component nature of the solar activity cycle and also for the main qualitative differences in the intensity and distribution of activity in the two components. The model provides for the formation of long lived coronal hole like magnetic structures during the declining years of the activity cycle. This might account for the third maximum in the indices of geomagnetic activity.