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The structure and variability of Mars upper atmosphere as seen in MAVEN/IUVS dayglow observations

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Academic year: 2021

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Figure

Table 1. Observations of Martian Dayglow From IUVS and Prior Missions
Figure 1. (top) The IUVS’s FUV and MUV detectors color composite generated using a full vertical scan from orbit 110 (2059 UTC, 18 October 2014), one of the 744 profiles
Figure 2. Mean altitude profiles for the CO + 2 ultraviolet doublet, CO Cameron band, OI 297.2 nm, and CO + 2 Fox- Fox-Duffendack-Barker bands for two solar longitudes and (top) SZA = 30–45 ∘ and (bottom) SZA = 50–70 ∘
Figure 3. Ratio of Cameron band and CO + 2 UVD for (left) L S = 218 ∘ and (right) L S ∼ 345 ∘ seasons and SZA = 30–45 ∘ (solid curves) and 50–70 ∘ (dashed curve)
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