Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p23b1708a&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P23B-1708
Physics
[5400] Planetary Sciences: Solid Surface Planets, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Martian surface temperatures are the results of radiative exchanges between the air and the shallow subsurface. Thermal inertia (TI) and the albedo are key parameters for modulating diurnal temperature variation of surfaces. TI, which represents the resistance to change in temperature of the upper few centimeters of the subsurface throughout the day, is independent of local time, latitude, and season. Thermal infrared spectrometers TES and THEMIS that measured the surface temperature have been frequently used to derive the thermal properties of the martian surface (see e.g. Putzig et al. 2005; Fergason et al. 2006). Global TI derivation techniques usually assume that the thermophysical properties of the soil are vertically uniform (Putzig et al. 2005), while vertical heterogeneities are observed (Putzig and Mellon 2007; Bandfield and Feldman 2008). As the thermal wave penetration depth varies with season, various apparent thermal inertias are derived as a function of season for a given location (Putzig et al. 2005). Surface temperatures (larger than ~200 K) can be derived from the OMEGA/Mars Express hyperspectral observations (Jouglet et al. 2007). Of special interest is the elliptical MEX orbit that makes possible to observe a given surface element at various local time and solar longitude. This allow us to explore different parts of the thermal response of martian soils and can be used to better constrain the properties of the subsurface. We have developed an operational pixel-to-pixel climate modeling interface using the Martian Global Climate Model (Forget et al. 1999), in order to compare the surface temperature measured by OMEGA with the modeled temperature. A systematic comparison data/model covering 4 Martian years will be discussed. A few local scale thermal inertia retrievals will be then presented and compared to previous studies based on TES/MGS and THEMIS/Mars Odyssey data. We will also investigate the thermophysical properties of soils where anomalous thermal behaviors have been spotted in the OMEGA observations.
Audouard J.
Bibring J.
Gondet Brigitte
Langevin Yves
Poulet François
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