Dynamic Mapping of Coronal Activity

There is a great deal of variation in how CMEs are manifested in EUV and coronagraph images. Complicating the issue is the range of CME-associated phenomena: shocks, waves, prominences, flares, dimmings, to name a few. None of these phenomena are a necessary or sufficient condition for a CME. However, each can provide clues as to CME origin, topology, and kinematics. New analysis strategies have been devised specifically to extract key properties of CMEs and CME-associated phenomena, with results that are converging towards a more consistent model of solar eruptive menagerie. We will discuss techniques such as Persistence Mapping and Time Convolution mapping, and how they are used to extract the dynamics of eruptive phenomena.