The occurrence and distribution of discrete and broadband ULF wave power

ULF waves are an important mechanism by which energy is transferred from the solar wind across the magnetopause and throughout the magnetosphere. Here, we investigate the occurrence and distribution of discrete ULF wave power in the inner magnetosphere using GOES magnetometer data from 2013-2016. This is achieved by adapting the novel AFINO time domain analysis code , originally designed to identify quasi-periodic signatures in solar flares to identify periods of discrete ULF wave activity at geosynchronous orbit . Using the results from AFINO we investigate the solar wind conditions most favorable to discrete ULF wave power versus broadband wave power, and examine the typical properties of discrete ULF waves, including their characteristic periods and mode types. We find that discrete ULF waves are predominantly poloidal mode waves which occur more commonly in the dawn and noon sectors during quiet solar wind conditions . Broadband ULF wave power is more dominant during enhanced solar wind conditions, while the total integrated ULF wave power is also increased during these times. These results have important implications for understanding how ULF waves transport energy throughout the magnetosphere either by wave-particle interactions via discrete resonances or radial transport via diffusion.