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This paper constrains the scattering phase function of water ice clouds(WICs) found within Mars' Aphelion Cloud Belt (ACB), determined from orbit byprocessing publicly available raw Mars Color Imager (MARCI) data spanning solarlongitudes (Ls) 42-170 during Mars Years (MYs) 28 and 29. MARCI visiblewavelength data were calibrated and then pipeline-processed to select thepixels most likely to possess clouds. Mean phase function curves for the MARCIblue filter data were derived, and for all seasons investigated, modeledaggregates, plates, solid and hollow columns, bullet rosettes, and droxtalswere all found to be plausible habits. Spheres were found to be the leastplausible, but still possible. Additionally, this work probed the oppositionsurge to examine the slope of the linear relationship between column ice watercontent and cloud opacity on Mars, and found a significant dependence onparticle radius. The half-width-half-maxima (HWHM) of the visible 180 degreepeak of five MARCI images were found to agree better with modeled HWHM for WICsthan with modeled HWHM for dust.

Aphelion Cloud Belt Phase Function Investigations with Mars Color Imager (MARCI)