Martian Meteoric Mg+: Atmospheric Distribution and Variability From MAVEN/IUVS

Since the discovery of atmospheric Mg+ on Mars in 2015 by the Mars Atmosphere and Volatile Evolution mission, there have been almost continuous observations of this meteoric ion layer in a variety of seasons, local times, and latitudes. Here, we present the most comprehensive set of observations of the persistent metal ion layer at Mars, constructing the first grand composite maps from pooled medians of subsamples of a metallic ion species. These maps demonstrate that Mg+ appears in almost all conditions when illuminated, with peak density values varying between 100 and 500 cm(-3), dependent on season and local time. There exists significant latitudinal variation within a given season, indicating that Mg+ is not simply an inert tracer, but may instead be influenced by the meteoric input distribution and/or atmospheric dynamics and chemistry. Geographic maps of Mg+ density as a function of latitude and longitude indicate the influence of atmospheric tides, and there is no apparent correlation with remnant crustal magnetic fields. This work also presents counter-intuitive results, such as a reduction of Mg+ ions in the northern hemisphere during Northern Winter in an apparent correlation with dust aerosols.

Automated summary

Since the discovery of atmospheric Mg+ on Mars in 2015, continuous observations of this meteoric ion layer have been conducted. This study presents the most comprehensive observations of the persistent metal ion layer, showing that Mg+ appears under various conditions with peak densities varying between 100 and 500 cm(-3). Significant latitudinal variation within a season suggests that Mg+ is influenced by meteoric input distribution and/or atmospheric dynamics and chemistry. Counter-intuitive results, such as a reduction of Mg+ ions during Northern Winter in the northern hemisphere, are also observed.