Authors: Richard Zhang (Cupertino High School and Stanford University), Wei Liu (Lockheed Martin Solar and Astrophysics Laboratory), Ruizhu Chen (Stanford University)

The magnetized solar corona hosts a variety of waves that can be observed in extreme ultraviolet (EUV) from space-borne telescopes. These waves can carry significant amount of energy to contribute to heating the solar corona. They also offer valuable clues for diagnosing the physical conditions on the Sun, using a technique called coronal seismology. Quasi-period fast-mode propagating wave trains (QFPs) are a relatively new observational phenomenon. They are usually associated with solar flares and/or coronal mass ejections (CMEs). We performed a systematic survey of QFPs using the EUV data from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) over its entire mission (2010-present). We will present the statistics on the occurrence of QFPs and their preferential association with certain types of solar activity. We will also report the statistical distributions of the wave characteristics, including their speeds, frequencies, amplitudes, and spatial extents. These measurements will provide a benchmark to allow these waves to be used as diagnostic tools for coronal seismology.