Venusian green line auroral emissions excited by solar energetic particles: Synergy with M-MATISSE mission

Previous ground-based observations have detected the Venusian green auroral emissions accompanied by the arrival of coronal mass ejections or corotating interaction regions at Venus, suggesting that their origins were solar energetic particles (SEPs). We simulated electron densities consistent with the VEx/VeRa radio occultation measurements and the green line emission brightness on the order of ~10-100 R in the nadir and ~1-10 kR in the limb. Our results support that the Venusian green line auroral emissions were excited by SEPs. Due to the similarity in the magnetic environment and composition of the upper atmosphere between Mars and Venus, we will show the feasibility of the Mars Aurora and Dust Camera (M-AC) for detecting green line auroral emissions on Mars during solar events. Simultaneous observations of the auroral images by M-AC, the particle flux by M-EPI, and the electron density by MaCro will provide radiation impacts on the Martian atmosphere.