Open AccessAphelion water‐ice cloud mapping and property retrieval using the OMEGA imaging spectrometer onboard Mars Express
Author(s) -
Madeleine J.B.,
Forget F.,
Spiga A.,
Wolff M. J.,
Montmessin F.,
Vincendon M.,
Jouglet D.,
Gondet B.,
Bibring J.P.,
Langevin Y.,
Schmitt B.
Publication year - 2012
Publication title -
journal of geophysical research: planets
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 1.67
H-Index - 298
eISSN - 2156-2202
pISSN - 0148-0227
DOI - 10.1029/2011je003940
Subject(s) - opacity , tharsis , mars exploration program , atmosphere of mars , ice cloud , atmospheric sciences , physics , remote sensing , environmental science , radiative transfer , geology , astrobiology , optics , martian
Mapping of the aphelion clouds over the Tharsis plateau 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 L s = 330° to MY29 L s = 180° and are acquired at various local times, ranging from 8 AM to 6 PM. Cloud maps of the Tharsis region constructed using the 3.1 μ m 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 3.5 μ m. The second group is characterized by particle sizes of ∼5 μ m which appear to be quite constant over L s 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 2.9 pr. μ m on average, and can reach 5.2 pr. μ m in the thickest clouds of Tharsis.