Io, the innermost Galilean satellite of Jupiter, is the most volcanically active body in the Solar System. Its atmosphere is primarily composed of SO₂, S, O, and SO, and is continuously bombarded by plasma from the Io torus at a relative velocity of ~ 60 km/s. As a result of this strong plasma–atmosphere interaction, Io constitutes a major source of neutrals for the Jovian magnetosphere, the ultimate source of its plasma and the main driver of its dynamics. Despite decades of observations and modeling efforts, many fundamental properties of Io’s atmosphere—its spatial distribution, temporal variability, and loss mechanisms—remain poorly constrained. As this is a promotion seminar, I will focus primarily on the big-picture description of the plasma–atmosphere interaction at Io. I will begin with a brief overview of the Jovian magnetosphere and the four Galilean satellites, before concentrating specifically on Io. I will then describe the complexity and diversity of the physical processes pertaining to Io’s plasma/atmosphere interaction and insist on its primordial role within the Jovian magnetospheric system. Finally, I will present my modeling approach to this interaction, based on multi-species physical chemistry, and briefly review selected publications that highlight my original contributions to the field, as well as outline directions for my future research
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