Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Details Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM Dust and cloud detection at the Mars limb with UV scattered sunlight with SPICAM

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jgre..11109s10r&link_type=abstract

Journal of Geophysical Research, Volume 111, Issue E9, CiteID E09S10

Physics

8

Atmospheric Composition And Structure: Aerosols And Particles (0345, 4801, 4906), Atmospheric Composition And Structure: Cloud/Radiation Interaction, Atmospheric Composition And Structure: Planetary Atmospheres (5210, 5405, 5704), Planetary Sciences: Solar System Objects: Mars

Scientific paper

The UV detector of Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) on board Mars Express has measured several profiles of light scattered at the limb of Mars. In this paper we present 33 profiles taken between January 2004 and August 2005. Scattering of UV light at the limb of Mars is due to the molecules of the atmosphere, dust particles, and sometimes cloud particles which appear as detached layers above the extended dust layer. We have used a radiative transfer model to retrieve the haze and cloud properties. Rough estimate of the particle size shows that both cloud particles and dust particles above 20 km are in the range 10 to 100 nm. Such particles are much smaller than micron-sized dust particles previously observed in the lower atmosphere, generally from landers. Gravitational segregation is thought to be responsible for these differences in particle size between low and high atmosphere.

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