Coronal Mass Ejections (CMEs), when aimed towards Earth, can cause geomagnetic storms which lead to a host of problems, including interference with radio communication, widespread blackouts, and endangering astronauts. We investigate the idea that the strongest CMEs may not leave the Sun alone, and that CMEs which interact before reaching Earth can cause more devastating geomagnetic storms. We use both in-situ data and remote data from the Wind and SOHO spacecraft, respectively, to identify potential interacting CMEs. Next, we employ a hydrodynamical numerical model to compare the speed and density profiles to those measured by Wind spacecraft. Then, we analyze the complexity of their structures using a wavelet transformation method. Finally, we present a list of these various structures to perform further analysis.

This work is supported by the NSF-REU Solar Physics program at SAO, grant number AGS-1850750.