Comparison of Global Martian Plasma Models in the Context of MAVEN Observations

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Details

Original languageEnglish
Pages (from-to)3714-3726
JournalJournal of geophysical research: Space physics
Volume123
Issue number5
Publication statusPublished - 2018
MoE publication typeA1 Journal article-refereed

Researchers

  • Hilary Egan
  • Yingjuan Ma
  • Chuanfei Dong
  • Ronan Modolo
  • Riku Järvinen

  • Stephen Bougher
  • Jasper Halekas
  • David Brain
  • James Mcfadden
  • John Connerney
  • David Mitchell
  • Bruce Jakosky

Research units

  • University of Colorado Boulder
  • University of California at Los Angeles
  • Princeton University
  • Universite Paris Saclay
  • University of Michigan, Ann Arbor
  • University of Iowa
  • University of California at Berkeley
  • NASA Goddard Space Flight Center
  • Finnish Meteorological Institute

Abstract

Global models of the interaction of the solar wind with the Martian upper atmosphere have proved to be valuable tools for investigating both the escape to space of the Martian atmosphere and the physical processes controlling this complex interaction. The many models currently in use employ different physical assumptions, but it can be difficult to directly compare the effectiveness of the models since they are rarely run for the same input conditions. Here we present the results of a model comparison activity, where five global models (single-fluid MHD, multifluid MHD, multifluid electron pressure MHD, and two hybrid models) were run for identical conditions corresponding to a single orbit of observations from the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. We find that low-altitude ion densities are very similar across all models and are comparable to MAVEN ion density measurements from periapsis. Plasma boundaries appear generally symmetric in all models and vary only slightly in extent. Despite these similarities there are clear morphological differences in ion behavior in other regions such as the tail and southern hemisphere. These differences are observable in ion escape loss maps and are necessary to understand in order to accurately use models in aiding our understanding of the Martian plasma environment.

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