Apparent thermal inertia and the surface heterogeneity of Mars

By Nathaniel E. Putzig, M. Mellon. 2007

368 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Physiology

View Paper: https://www.semanticscholar.org/paper/daa9b561d7c3cff91fcbf1afc419a0d40f03c155

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In Astronomy and Astrophysics

1. E. Komatsu
2. Volker Springel
3. David N. Spergel
4. Simon D. M. White
5. Mark Halpern
6. C. Bennett
7. Andrey V. Kravtsov
8. J. Weiland

In Physiology

1. Ehouarn Millour
2. Michael D. Smith
3. Francois Forget
4. A. S. McEwen
5. B. Hynek
6. C. Dundas
7. S. Diniega
8. M. Hoke

Citations in the corpus

• THE MARTIAN ATMOSPHERIC BOUNDARY LAYER (2011, methodology): “Surface static data are extracted from maps derived from recent Martian spacecraft measurements, such as the 64 pixel per degree (ppd) MOLA topography [Smith et al., 2001], 8 ppd MGS TES albedo [Christensen et al., 2001] and 20 ppd TES thermal inertia [Putzig and Mellon, 2007].”
• Long-term monitoring of martian gully formation and evolution with MRO/HiRISE (2015, methodology): “…topography (using the global Digital Elevation Model, providing information about the regional setting rather than a specific morphologic feature of the landforms), Thermal Emission Spectrometer (TES) albedo (Christensen et al., 2001), and TES-derived thermal inertia (Putzig and Mellon, 2007).”
• Formation timescales of large Martian valley networks (2011, methodology): “Using MGS Thermal Emission Spectrometer (TES) thermal inertia data (Putzig and Mellon, 2007) to determine grain size (e.g. Pelkey et al., 2001; Presley and Christensen, 1997) within these valleys produced median grain sizes of up to a few hundred micrometers in diameter, typical of sand.”
• Initial results from the thermal and electrical conductivity probe (TECP) on Phoenix (2010, methodology): “Figure 13. Daytime (gray) and nighttime (black) thermal inertia values derived from TECP (circles) and Mars Global Surveyor Thermal Emission Spectrometer observations (crosses [ Putzig and Mellon, 2007 ]).”
• Selection of the Mars Science Laboratory Landing Site (2012, methodology): “Thermal differencing rock abundance estimates from IRTM (1 pixel per degree) and TES (8 pixels per degree) for the landing sites are higher than those measured in HiRISE images.”
• Eight-year climatology of dust optical depth on Mars (2014, background): “Dust climatologies are also commonly used as input values for atmospheric species and surface quantity retrievals, e.g. atmospheric ozone (Clancy et al., 2014), surface albedo (Vincendon et al., 2014), and surface thermal inertia (Putzig and Mellon, 2007), to cite only a few.”
• SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: PLANETS AND CELESTIAL CALIBRATION SOURCES (2010, background): “Additionally, the Martian surface is itself far from homogenous, with polar ice-caps of changing extent and variations in albedo and thermal inertia on relatively small scales (Putzig & Mellon 2007; Christensen et al. 2001).”