Kinematics Analysis of Coronal Mass Ejection-Driven Compression Waves Using EUV Observations

oronal mass ejections (CMEs) often drive compressions or shock waves in the solar corona. Such compressions and shocks are thought to accelerate large fluxes of solar energetic particles (SEPs). The study of the fronts is important for modeling the acceleration of particles in the corona. These transient features may be observed in extreme ultraviolet (EUV) light as large-scale propagating fronts. In order to accurately measure and analyze these fronts, we use SDO/AIA data. Base difference data were created about 120 CME/shock event candidates from 2010 to 2016, and about 25 of the clearest events were analyzed manually. The best events were on the limb of the Sun, with little other ejecta obscuring the view of the compression. Because the waves are relatively very dim, we developed a special procedure for correctly identifying and enhancing their intensity. After removing noise and non-physical bright features, we used Savitsky-Golay and Gaussian smoothing to guide the selection of the front, back, and peak of each front over the period of the event. The data was saved, used to measure the radial and lateral evolution of EUV wave events, and analyzed to obtain kinematics, intensity, and wave thickness information. We present the statistical summary of our findings. These detailed measurements form the basis of our comprehensive analysis of UV wave properties and their ability to accelerate energetic particles.