Variation of the Martian Ionospheric Electron Density from Mars Express Radar Soundings

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First measurements of composition and dynamics of the Martian ionosphere by MAVEN's Neutral Gas and Ion Mass Spectrometer (2015, background): “It is also consistent with the observations of Mars Express of the peak altitude at SZA< 10° being less (but close to) 130 km [Morgan et al., 2008; Němec et al., 2011].”
A review of observed variability in the dayside ionosphere of Mars (2009, methodology): “It is also possible to determine the vertical profile of electron density between the spacecraft (whose altitude during MARSIS operations is typically between 275 km and 1200 km) and the maximum electron density (whose altitude is variable, but on the order of 130 km) (Nielsen et al., 2006; Morgan e”
Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere (2015, background): “These variations are likely generated by a combination of planetary and tidal waves launched in the lower atmosphere that propagate to thermospheric heights [e.g., Forbes et al., 2003; Wilson, 2002; Moudden and Forbes, 2008, 2010].”
Three‐dimensional Martian ionosphere model: I. The photochemical ionosphere below 180 km (2013, background): “However, several authors [Hantsch and Bauer, 1990; Gurnett et al., 2005; Withers and Mendillo, 2005; Fox and Yeager, 2006; Morgan et al., 2008; Sánchez-Cano et al., 2013] have overcome this limitation by fitting analytic functions to the observed profiles.”