Fig. 5: Results from our 3D-MHD simulation model for the case in which the planet possesses an intrinsic dynamo (Case–I). | Communications Earth & Environment

Fig. 5: Results from our 3D-MHD simulation model for the case in which the planet possesses an intrinsic dynamo (Case–I).

From: Terrestrial atmospheric ion implantation occurred in the nearside lunar regolith during the history of Earth’s dynamo

Fig. 5: Results from our 3D-MHD simulation model for the case in which the planet possesses an intrinsic dynamo (Case–I).The alt text for this image may have been generated using AI.

a Total number density plot depicting the large-scale structure of the wind-atmosphere interaction up to the lunar orbit in the quasi-steady state. b Polar-cut view of the topology of the planet’s magnetosphere when it is impinged by magnetized solar wind. Quivers represent the magnetic field. c 2D slice of the normalized solar wind number flux in the lunar orbital plane. The flux drops by ~4 orders of magnitude inside the magnetotail compared to the shocked solar wind region between the bow shock and the magnetopause boundary, where it exhibits a sharp gradient. d Terrestrial atmospheric number flux in the magnetotail region. The quiver arrows denote the plane-projected bulk velocity component, indicating the escaping pathways. The filled white circle representing the planet’s core is not included in the passive advective tracers.

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