P046-0012
Magnetic depressions in the Martian magnetosheath and upstream solar wind

Friday, 11 December 2020
Poster
Hadi Madanian1, Tomas Karlsson2, Rudy A Frahm1, Jasper S Halekas3, Christian Mazelle4 and Nick Omidi5, (1)Southwest Research Institute, San Antonio, TX, United States, (2)KTH Royal Institute of Technology, Stockholm, Sweden, (3)University of Iowa, Department of Physics and Astronomy, Iowa City, IA, United States, (4)IRAP, University of Toulouse, CNRS, UPS, CNES, Toulouse, France, (5)Solana Scientific Inc, Solana Beach, CA, United States
Abstract:
Magnetic depressions or magnetic holes have been observed upstream of Mars. They are characterized by low magnetic field strength correlated with enhanced plasma density and/or temperature, and they can have a higher momentum than the ambient solar wind plasma. At Mercury, these structures can survive the bow shock and travel through the magnetosheath in the form of diamagnetic plasmoids. In this study, we discuss the plasma properties of magnetic holes in the solar wind upstream of Mars, and within the Martian magnetosheath.
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