Existence, magnitude, and cross-planet comparison of Martian magnetosheath asymmetries

Determine whether the Martian magnetosheath exhibits significant asymmetries in the spatial distributions of magnetic field strength and plasma properties—including solar wind proton density and velocity and planetary oxygen ion densities—between the quasi-parallel and quasi-perpendicular magnetosheaths; quantify the magnitude of any such asymmetries; and compare them to analogous asymmetries observed at other planets.

Background

The authors note that, while individual asymmetric features at Mars have been reported (e.g., sheath thickness, electron temperature, magnetic field draping), a comprehensive understanding of asymmetries within the Martian magnetosheath is lacking. In contrast, Earth’s magnetosheath properties are well documented and strongly dependent on shock geometry, and Venus shows both similarities and differences. Establishing whether Mars displays comparable asymmetries—and quantifying and contextualizing them relative to other planets—would illuminate the universality and planet-specific drivers of magnetosheath behavior.

This problem is framed explicitly in the introduction as an unresolved set of questions motivating the paper, indicating a need for systematic, quantitative assessment across magnetic field and plasma variables, including contributions from both solar wind and planetary ions.