Abstract
The interaction between the magnetized stellar wind plasma and the hydrodynamic flow from the upper atmosphere of a non-magnetic exoplanet is studied. The recently discovered warm Neptune TOI-421c is considered as an example of such an interaction. The obstacle boundary is determined by the condition of pressure balance between the stellar wind and the expanded atmosphere. Extreme ultraviolet stellar radiation drives a hydrodynamic supersonic outflow of hydrogen atoms. Neutral atmospheric atoms penetrate the region of the stellar wind, where they are ionized and mixed with the stellar wind plasma. The 3D MHD model was applied to calculate the detached bow shock and the magnetosheath region between the shock and the streamlined surface-ionopause. We have obtained a thick magnetic barrier, characterized by a strong increase in the magnetic field and total pressure, a decrease in the velocity, pressure and temperature of the plasma. An enhanced magnetic field shifts the ionopause towards the planet.
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This work is supported by the Krasnoyarsk Mathematical Center, financed by the Ministry of Science and Higher Education of the Russian Federation in the framework of the establishment and development of regional Centers for Mathematics Research and Education (Agreement No. 075-02-2023-912).
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Erkaev, N.V., Gorbunova, K.D. (2023). Magnetic Barrier in Front of Exoplanets Interacting with Stellar Wind. In: Kosterov, A., Lyskova, E., Mironova, I., Apatenkov, S., Baranov, S. (eds) Problems of Geocosmos—2022. ICS 2022. Springer Proceedings in Earth and Environmental Sciences. Springer, Cham. https://doi.org/10.1007/978-3-031-40728-4_18
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