Analysis, Interpretation, and Modeling of Mars Dayglow Spectra

Introduction: The Mariner 6 and 7 (1969), Mariner 9 (1971), and Viking 1 and 2 (1975) missions provided the first quantitative details about the structure and energetics of the Mars atmosphere [1-8]. These limited data sets supplied the observational foundation for the current semiempirical reference atmospheric models [2, 10-13]. Not until more than 20 years later did new generations of landers and orbiters begin to revisit the planet [14-24]. The Mariner spacecraft had UV spectrometers that recorded limb scans of the Mars dayglow spectrum, shown in Figure 1, versus tangent ray height. The primary objective of the work reported here is comparative analysis, interpretation, and modeling of the altitude profiles of the Mars dayglow as recorded during the Mariner and Mars Express (MEX) Missions.