Aphelion water-ice cloud mapping and property retrieval using the OMEGA imaging spectrometer onboard Mars Express

Jean-Baptiste Madeleine (1) , Francois Forget (1, 2) , Aymeric Spiga (1) , Michael J. Wolff (3) , Franck Montmessin (4) , Mathieu Vincendon (5) , Denis Jouglet (5) , Brigitte Gondet (5) , Jean-Pierre Bibring (5) , Yves Langevin (5) , Bernard Schmitt (6)

1 LMD - Laboratoire de Météorologie Dynamique (UMR 8539)
2 IPSL - Institut Pierre-Simon-Laplace
3 SSI - Space Science Institute [Boulder]
4 PLANETO - LATMOS
5 IAS - Institut d'astrophysique spatiale
6 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble

Mapping of the aphelion clouds over Tharsis and retrieval of their particle size and visible opacity are made possible by the OMEGA imaging spectrometer aboard Mars Express. Observations cover the period from MY26 Ls=330{degree sign} to MY29 Ls=180{degree sign} and are acquired at various local times, ranging from 8AM to 6PM. Cloud maps of the Tharsis region constructed using the 3.1µm ice absorption band reveal the seasonal and diurnal evolution of aphelion clouds. Four distinct types of clouds are identified: morning hazes, topographically controlled hazes, cumulus clouds and thick hazes. The location and time of occurrence of these clouds are analyzed and their respective formation process is discussed. An inverse method for retrieving cloud particle size and opacity is then developed and can only be applied to thick hazes. The relative error of these measurements is less than 30% for cloud particle size and 20% for opacity. Two groups of particles can be distinguished. The first group is found over flat plains and is composed of relatively small particles, ranging in size from 2 to 3.5µm. The second group is characterized by particle sizes of ~5µm which appear to be quite constant over Ls and local time. It is found west of Ascraeus and Pavonis Mons, and near Lunae Planum. These regions are preferentially exposed to anabatic winds, which may control the formation of these particles and explain their distinct properties. The water ice column is equal to 2.9pr.µm on average, and can reach 5.2pr.µm in the thickest clouds of Tharsis.

Mots clés: Mars; Microphysics; Clouds; Aerosols; Near-infrared spectrometry; Radiative transfer

Domaines: Planétologie et astrophysique de la terre [astro-ph.EP]; Planétologie et astrophysique de la terre [astro-ph.EP]; Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]; Instrumentation et méthodes pour l'astrophysique [astro-ph.IM]

Jean-Baptiste Madeleine, Francois Forget, Aymeric Spiga, Michael J. Wolff, Franck Montmessin, et al.. Aphelion water-ice cloud mapping and property retrieval using the OMEGA imaging spectrometer onboard Mars Express. Journal of Geophysical Research. Planets, 2012, 117 (E11), pp.E00J07. ⟨10.1029/2011JE003940⟩. ⟨hal-00678749⟩