High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications

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THE MARTIAN ATMOSPHERIC BOUNDARY LAYER (2011, background): “been, applied to flows with unstable stratification and strong convection, Forget et al. [1999] express some doubts about the validity of the model in such conditions.”
Apparent thermal inertia and the surface heterogeneity of Mars (2007, methodology): “…determined from visible-band observations and as derived from temperature data in tandem with thermal inertia (Kieffer et al., 1977; Palluconi and Kieffer, 1981; Fergason et al., 2006a, 2006b) are also suggestive of surface heterogeneity, but have never been fully explained (Hayashi et al., 1995).”
The Sedimentary Rock Record of Mars: Distribution, Origins, and Global Stratigraphy (2012, background): “Similarly, thermal inertia values for stratified deposits in Hebes Chasma are too low to be consistent with well-lithified rock and are more consistent with poorly cemented or highly porous eolian or volcanic sediments (Fergason et al. 2006).”
Selection of the Mars Science Laboratory Landing Site (2012, methodology): “…critical for navigating the spacecraft to the correct entry point, (3) global TES thermal inertia data at 3 km/pixel (Putzig et al. 2005; Putzig and Mellon 2007), (4) THEMIS thermal inertia data at 100 m/pixel (Fergason et al. 2006a, this issue), and (5) MRO image data from HiRISE, CTX and CRISM.”