EGU21-9157
https://doi.org/10.5194/egusphere-egu21-9157
EGU General Assembly 2021
© Author(s) 2021. This work is distributed under
the Creative Commons Attribution 4.0 License.

Dynamics of the Martian bow shock location

Philippe Garnier1, Christian Jacquey1, Vincent Génot1, Beatriz Sanchez-Cano2, Xavier Gendre3, Christian Mazelle1, Xiaohua Fang4, Jacob R Gruesbeck5,6, Benjamin Hall7, Jasper S Halekas8, and Bruce M Jakosky4
Philippe Garnier et al.
  • 1IRAP, Universite Toulouse 3, IRAP, Toulouse, France (philippe.garnier@irap.omp.eu)
  • 2Physics and Astronomy Department, University of Leicester, Leicester, UK
  • 3ISAE-SUPAERO, Université de Toulouse, France
  • 4Laboratory for Atmospheric and Space Physics University of Colorado, Boulder, US
  • 5Department of Astronomy, University of Maryland, College Park, MD, US
  • 6NASA Goddard Space Flight Center, Greenbelt, MD, US
  • 7Space & Planetary Physics Group, Department of Physics, Lancaster University, Lancaster, UK
  • 8Department of Physics and Astronomy, University of Iowa, Iowa City, Iowa, USA

The Martian interaction with the solar wind is unique due to the influence of multiple internal and external drivers, including remanent crustal magnetic fields that make the interaction unique. In this work we focus on the analysis of the dynamics of the plasma boundaries that shape the interaction of the planet with its environment, and in particular of the shock whose location varies in a complex way. We use multi spacecraft datasets from three missions (Mars Global Surveyor, Mars Express, Mars Atm-osphere and Volatile Evolution) to provide a coherent picture of the shock drivers. We show how the use of different statistical parameters or cross correlations may modify conclusions. We thus propose the use of refined methods, such as partial correlation analysis or Akaike Information Criterion approach to analyse the multiple drivers of the shock location and rank their relative importance: solar wind dynamic pressure, extreme ultraviolet fluxes, magnetosonic mach number, crustal magnetic fields, but also solar wind orientation parameters. Seasonal effects of crustal fields on the shock, through ionospheric coupling, are also investigated.

How to cite: Garnier, P., Jacquey, C., Génot, V., Sanchez-Cano, B., Gendre, X., Mazelle, C., Fang, X., Gruesbeck, J. R., Hall, B., Halekas, J. S., and Jakosky, B. M.: Dynamics of the Martian bow shock location, EGU General Assembly 2021, online, 19–30 Apr 2021, EGU21-9157, https://doi.org/10.5194/egusphere-egu21-9157, 2021.

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