High-Resolution Thermal Inertia Mapping from the Mars Global Surveyor Thermal Emission Spectrometer

By M. Mellon, B. Jakosky, Hugh H. Kieffer, Philip R. Christensen. 2000

555 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/cc25e728c7047f1cfdaa3abfceaaf0df26bf0112

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Philip R. Christensen
2. V. Hamilton
3. Michael D. Smith
4. J. Bandfield
5. Francois Forget
6. M. Mellon
7. H. McSween
8. Nathaniel E. Putzig

In Atmospheric Science

1. Michael D. Smith
2. V. Hamilton
3. Philip R. Christensen
4. J. Bandfield
5. M. Mellon
6. Francois Forget
7. Nathaniel E. Putzig
8. R. Clancy

Citations in the corpus

• Sequence of infilling events in Gale Crater, Mars: Results from morphology, stratigraphy, and mineralogy (2013, background): “A surface characterized by a thermal inertia ≤200SI is usually interpreted as fine-grained and/or unconsolidated material [Mellon et al., 2000].”
• THE MARTIAN ATMOSPHERIC BOUNDARY LAYER (2011, background): “These include the surface temperature Ts, which itself depends on the thermal inertia (I) and on the albedo (a) of the surface material [Kieffer et al., 1976, 1977; Mellon et al., 2000; Christensen et al., 2001; Fergason et al., 2006].”
• Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) (2007, background): “[132] The surface layer of Mars is globally dominated by soil deposits [Palluconi and Kieffer, 1981; Christensen and Moore, 1992; Mellon et al., 2000].”
• Assimilation of thermal emission spectrometer atmospheric data during the Mars Global Surveyor aerobraking period (2007, methodology): “A new surface thermal inertia field was also employed, derived from TES data (Mellon et al., 2000) between 30◦S and 60◦N, blended with Viking observations from 60◦S to 30◦S (Palluconi and Kieffer, 1981) and in the polar regions (Paige et al.”
• Global mineral distributions on Mars (2002, background): “Thermal inertia is moderate ( 200–350 J m 2 K 1 s 1/2) [Mellon et al., 2000] and is also not distinct from the surrounding area.”
• 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).”
• Formation of Martian Gullies by the Action of Liquid Water Flowing Under Current Martian Environmental Conditions (2005, methodology): “On the basis of the measured TES thermal inertia (I) at each gully site as well as modeled mean surface temperatures (To) [Mellon et al., 2000], Heldmann and Mellon [2004] computed the subsurface temperature at the depth of each individual alcove base.”
• Mars: Nature and evolution of young latitude‐dependent water‐ice‐rich mantle (2002, background): “The regions of circumpolar mantles, at least, their lowerlatitude parts, are characterized by moderate values of thermal inertia [e.g., Mellon et al., 2000], while bare compact deposits with ice-filled pores would have extremely high thermal inertia.”
• Selection of the InSight Landing Site (2017, methodology): “H. Silverman, S. Ferry, M. Caplinger, M. Ravine (2004) The Thermal Emission Imaging System (THEMIS) for the Mars 2001 Odyssey mission, Space Sci.”
• Equatorial and midlatitude distribution of chlorine measured by Mars Odyssey GRS (2007, unknown): “[Christensen, 1986a, 1986b; Mellon et al., 2000; Putzig et al., 2005].”
• Thermal inertia of near-Earth asteroids and implications for the magnitude of the Yarkovsky effect (2007, background): “about 400 J m s K (Mellon et al., 2000; Christiansen et al., 2003), that of bare rock is larger than 2500 J m s K (Jakosky, 1986), whereas the thermal inertia of metal rich asteroidal fragments can be larger than 12000 J m s K (Farinella et al.”
• Physical properties of the Mars Exploration Rover landing sites as inferred from Mini‐TES–derived thermal inertia (2006, methodology): “Some previous thermal inertia data sets, such as TES, used a single-point method to calculate thermal inertia values [Jakosky et al., 2000; Mellon et al., 2000].”