Mapping water ice clouds on Mars with MRO/MARCI

• Published in: Icarus (New York, N.Y. 1962) Vol. 332; pp. 24 - 49
• Main Authors: Wolff, Michael J., Clancy, R. Todd, Kahre, Melinda A., Haberle, Robert M., Forget, François, Cantor, Bruce A., Malin, Michael C.
• Format: Journal Article
• Language: English
• Published: Elsevier Inc 01.11.2019; Elsevier
• Subjects: Atmosphere; Atmospheric and Oceanic Physics; Mars; Physics; Radiative transfer; Ultraviolet observations; Mars; Radiative transfer; Atmosphere; Ultraviolet observations
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2019.05.041

Observations by the Mars Color Imager (MARCI) onboard the Mars Reconnaissance Orbiter (MRO) in the ultraviolet (UV, Band 7; 320 nm) are used to characterize the spatial and temporal behavior of atmospheric water ice over a period of 6 Mars Years. Exploiting the contrast of the bright ice clouds to the low albedo surface, a radiative transfer-based retrieval algorithm is developed to derive the column-integrated optical depth of the ice (τice). Several relatively unique input products are created as part of the retrieval development process, including a zonal dust climatology based on emission phase function (EPFs) sequences from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), a spatially variable UV-reflectance model for Band 7 (as well as for Band 6, 260 nm), and a water ice scattering phase function based on a droxtal ice habit. Taking into account a radiometric precision of 7%, an error analysis estimates the uncertainty in τice to be ∼0.03 (excluding particle size effects, which are discussed separately). Zonal trends are analyzed over the full temporal extent of the observations, looking at both diurnal and interannual variability. The main (zonal) features are the aphelion cloud belt (ACB) and the polar hoods. For the ACB, there can be an appreciable diurnal change in τice between the periods of 14h30–15h00 and 15h00–15h30 Local True Solar Time (LTST). The amplitude of this effect shows relatively large interannual variability, associated mainly with changes in the earlier time block. When averaged over the interval 14h00–16h00 LTST, the interannual differences in the ACB structure are appreciably smaller. When the MARCI τice are compared to those from the Thermal Emission Spectrometer (TES), there is a good correlation of features, with the most significant difference being the seasonal (LS) evolution of the ACB. For TES, the ACB zonal profile is relative symmetric about LS = 90°. In the MARCI data, this profile is noticeably asymmetric, with the centroid shifted to later in the northern summer season (LS = 120°). The MARCI behavior is consistent with that observed by several other instruments. The correspondence of MARCI τice zonal and meridional behaviors with that predicted by two Global Circulation Models (GCM) is good. Each model captures the general behavior seen by MARCI in the ACB, the polar hoods, and the major orographic/topographic cloud features (including Valles Mariners). However, the mismatches between GCM results and MARCI reinforce the challenging nature of water ice clouds for dynamical models. The released τice are being archived at Malin Space Science Systems at https://www.msss.com/mro_marci_iceclouds/. •The zonal behavior is dominated by aphelion cloud belt (ACB) and polar hood structures.•The MARCI ACB can demonstrate appreciable diurnal change and annual variability.•MARCI ACB observations show differences with those of Thermal Emission Spectrometer.•Dynamical models can capture the general behavior seen by the MARCI ACB and polar hoods.