MGS Radio Science electron density profiles: Interannual variability and implications for the Martian neutral atmosphere

By S. Bougher, S. Engel, D. Hinson, J. Murphy. 2004

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View Paper: https://www.semanticscholar.org/paper/80752e64e1c191e5894d16ab889a4b49f3e03094

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In Astronomy and Astrophysics

Citations in the corpus

Three‐dimensional Martian ionosphere model: I. The photochemical ionosphere below 180 km (2013, background): “The SZA variability simulated by the model is in good agreement with that fitted to MARSIS observations up to SZA 100ı. [64] The comparison with the results of another thermospheric/ionospheric GCM, the MTGCM [Bougher et al., 2004] shows that the SZA variability of the peak electron density and the ”
First measurements of composition and dynamics of the Martian ionosphere by MAVEN's Neutral Gas and Ion Mass Spectrometer (2015, background): “NGIMS OBSERVATIONS OF MARS’ IONOSPHERE 8960 longitude, and solar activity [Hantsch and Bauer, 1990; Bougher et al., 2004; Fox and Yeager, 2006; Morgan et al., 2008; Němec et al., 2011; Fox and Weber, 2012; Peter et al., 2014; Fallows et al., 2015; Zhang et al., 2015].”
Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere (2015, methodology): “This coupled configuration permits both thermal- and large-scale dynamical processes to be linked across the lower and upper atmospheres of Mars [Bougher et al., 2004, 2006, 2009].”
Polar warming in the Mars thermosphere: Seasonal variations owing to changing insolation and dust distributions (2006, methodology): “[9] The Mars Thermospheric General Circulation Model (MTGCM) itself is a finite difference primitive equation model that self-consistently solves for time-dependent neutral temperatures, neutral-ion densities, and three component neutral winds over the globe [see Bougher et al., 1999, 2004].”
Martian dayglow as seen by the SPICAM UV spectrograph on Mars Express (2006, methodology): “Radio occultation methods have been used to explore the Mars upper atmosphere and provide the electron density profile between 75 and 250 km in altitude [Bougher et al., 2001, 2004; Pätzold et al., 2005].”