Because it lacks a global magnetic field, Mars's atmosphere is subject to direct interaction with the solar wind, which can provide energy for atmospheric constituents to escape the planet's gravitational pull through a variety of processes, including photochemical escape, sputtering, and pick up ion escape Lillis et al., 2015). Evidence suggests that this solar wind interaction has played a major role in changing Mars from a warm, water rich environment to the cold, dry planet we observe today (Jakosky et al., 2018). Mars's atmosphere is comprised primarily of CO 2 but also exhibits a hydrogen corona that extends past the planet's bow shock (Anderson, 1974;Anderson & Hord, 1971). This hydrogen corona is subject to direct interaction with the solar wind by means of charge exchange, providing us with a unique laboratory to observe and characterize various phenomena within the upper Martian atmosphere.As solar wind protons propagate toward Mars, they can charge exchange with neutral hydrogen atoms in the planet's corona, resulting in energetic neutral atoms (ENAs) with the solar wind speed (Kallio et al., 1997). These ENAs can then travel toward the planet without being affected by electromagnetic forces and thus