Global thermal inertia and surface properties of Mars from the MGS mapping mission

By Nathaniel E. Putzig, M. Mellon, K. Kretke, R. Arvidson. 2005

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View Paper: https://www.semanticscholar.org/paper/db65d2170a824055e0f2fbed5443020ae66ffcd8

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In Astronomy and Astrophysics

Citations in the corpus

The High Resolution Imaging Science Experiment (HiRISE) during MRO’s Primary Science Phase (PSP) (2010, methodology): “Tools useful for coregistration of MOLA elevations with HiRISE images are described by Kolb and Okubo (in press).”
Selection of the InSight Landing Site (2017, background): “…and albedo data show a mode with thermal inertias less than 100 J m−2 K−1 s−1/2 and albedo higher than 0.25 that corresponds with these very dusty surfaces (Putzig et al. 2005; Mellon et al. 2008) that could be meters (Christensen and Moore 1992) to tens of meters thick (Mangold et al. 2009).”
High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, background): “represent areas composed of very fine surface dust [Putzig et al., 2005].”
Gusev crater: Wind‐related features and processes observed by the Mars Exploration Rover Spirit (2006, methodology): “The model uses MGCM results for lateral boundary conditions, and surface characteristics derived from MGS, including Mars Orbiter Altimeter (MOLA) 1/32� gridded topography, Thermal Emission Spectrometer thermal inertia [ Putzig et al., 2005 ] and albedo at 1/20� and 1/8� resolution, respectively.”
Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, background): “…of large surface areas having sufficiently high thermal inertia to infer that they represent materials in the form of coarse particulates to nearbedrock, which eliminates particle size effects (e.g., Christensen, 1982; Presley and Christensen, 1997; Mellon et al., 2000; Putzig et al., 2005).”
Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, methodology): “region of low thermal inertia [Mellon et al., 2000; Putzig et al., 2005] and it is plausible that hydrated minerals are”
Concentration of H, Si, Cl, K, Fe, and Th in the low- and mid-latitude regions of Mars (2007, background): “These areas have similar reflectance spectra [Putzig et al., 2005], but are significantly different in chemical”
Equatorial and midlatitude distribution of chlorine measured by Mars Odyssey GRS (2007, background): “Dusty regions have been proposed for areas with lower thermal inertia and higher albedo [Christensen, 1986a, 1986b; Mellon et al., 2000; Putzig et al., 2005 ].”
Geologic history of Mars (2010, background): “Olivine is detected almost everywhere in orbital spectra of the Hesperian plains where dust is sparse or absent (Christensen et al., 2001; Putzig et al., 2005), which likely implies only limited chemical weathering.”
Selection of the Mars Science Laboratory Landing Site (2012, background): “6) sample the moderate to high thermal inertia and intermediate to high albedo unit C that is dominated by crusty, cloddy, blocky or frozen soils (duricrust) with various abundances of rocks and bright dust (Golombek et al. 2008b, 2009b; Jakosky and Christensen 1986; Christensen and Moore 1992; Moor”
Stability and exchange of subsurface ice on Mars (2005, methodology): “[39] Temperatures are obtained with a one-dimensional thermal model of the subsurface, using thermal inertia map [Putzig et al., 2005], albedo map [Christensen et al., 2001], orbital elements [Allison and McEwen, 2000], and partial surface pressures obtained from the Thermal Emission Spectrometer…”
Apparent thermal inertia and the surface heterogeneity of Mars (2007, methodology): “The TES instrument’s downtrack smear of 5.4 km (see Putzig et al., 2005) and longitudinal variations within each observation ensure that any given observation does not fall entirely within a single map pixel, even at low latitudes.”
The Sedimentary Rock Record of Mars: Distribution, Origins, and Global Stratigraphy (2012, background): “…minerals in outcrops of stratified light-toned materials (Gendrin et al. 2005); thermal inertia of stratified materials (Christensen et al. 2001, Putzig et al. 2005, Fergason et al. 2006, Edwards et al. 2009); and observation of probable cements and diagenetic fronts in outcrop (Grotzinger et…”
Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect (2007, background): “Knowledge of the thermal inertia of asteroids is thus important for a number of reasons: (a) It can be used to infer the presence or absence of loose material on the surface: thermal inertia of fine dust is very low: ~30 J m s K (Putzig et al., 2005); lunar regolith, a layer of fragmentary incoheren”