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Stellar wind and photon radiation interactions with a planet can causeatmospheric depletion, which may have a potentially catastrophic impact on aplanet's habitability. While the implications of photoevaporation onatmospheric erosion have been researched to some degree, studies of theinfluence of the stellar wind on atmospheric loss are in their infancy. Here,we use three-dimensional magnetohydrodynamic simulations to model the effect ofthe stellar wind on the magnetosphere and outflow of a hypothetical planet,modeled to have an H-rich evaporating envelope with a pre-defined mass lossrate, orbiting in the habitable zone close to a low-mass M dwarf. We take theTRAPPIST-1 system as a prototype, with our simulated planet situated at theorbit of TRAPPIST-1e. We show that the atmospheric outflow is dragged andaccelerated upon interaction with the wind, resulting in a diverse range ofplanetary magnetosphere morphologies and plasma distributions as local stellarwind conditions change. We consider the implications of the wind-outflowinteraction on potential hydrogen Lyman-alpha (Lya) observations of theplanetary atmosphere during transits. The Lya observational signatures dependstrongly on the local wind conditions at the time of the observation and can besubject to considerable variation on timescales as short as an hour. Ourresults indicate that observed variations in exoplanet Lya transit signaturescould be explained by wind-outflow interaction.

Stellar Winds Drive Strong Variations in Exoplanet Evaporative Outflows and Transit Absorption Signatures