2007
DOI: 10.1029/2006je002798
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Rock abundance on Mars from the Thermal Emission Spectrometer

Abstract: [1] Nighttime infrared spectral observations returned from the Mars Global Surveyor Thermal Emission Spectrometer (TES) are well suited for determining the subpixel abundance of rocks on the surface of Mars. The algorithm used here determines both the areal fraction of rocky material and the thermal inertia of the fine-grained nonrock component present on the surface. Rock is defined as any surface material that has a thermal inertia !1250 J m À2 K À1 s À1/2 . This can be bedrock, boulders, indurated sediments… Show more

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Cited by 96 publications
(118 citation statements)
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References 68 publications
(148 reference statements)
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“…2). Areas inside the Vallis Marineris canyons and outflow troughs meet these constraints, but placing 150 km by 30 km ellipses on smooth, flat surfaces is problematical and rock abundance in global thermal differencing data sets far exceed 10 % (Christensen 1986;Nowicki and Christensen 2007). In addition, experience searching for low-wind MER ellipses in the equatorial latitudes has shown that this area is on storm tracks from weather systems generated at high northern latitudes (Golombek et al 2003a and Sect.…”
Section: Sites Identified During Discovery Proposal Preparationmentioning
confidence: 99%
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“…2). Areas inside the Vallis Marineris canyons and outflow troughs meet these constraints, but placing 150 km by 30 km ellipses on smooth, flat surfaces is problematical and rock abundance in global thermal differencing data sets far exceed 10 % (Christensen 1986;Nowicki and Christensen 2007). In addition, experience searching for low-wind MER ellipses in the equatorial latitudes has shown that this area is on storm tracks from weather systems generated at high northern latitudes (Golombek et al 2003a and Sect.…”
Section: Sites Identified During Discovery Proposal Preparationmentioning
confidence: 99%
“…Immediately after selection, a large number of landing site activities were initiated. The first Latitude and longitude in°, positive north and east, planetocentric; elevation in m with respect to MOLA geoid from Smith et al (2001aSmith et al ( , 2001b; TES thermal inertia in J m −2 K −1 s −1/2 from Mellon et al (2000); TES and IRTM rock abundance in % from Christensen (1986) and Nowicki and Christensen (2007), with values in parentheses partially in ellipse; Dust cover index from Ruff and Christensen (2002); albedo from Christensen et al (2001) and most important was to begin high-resolution imaging of the InSight ellipses with CTX and HiRISE on MRO. However, because the western Elysium region is directly north of Gale crater, about 600 km from where Curiosity was operating, there was a conflict between relaying information from Curiosity and imaging so close in time on the same orbital pass.…”
Section: First Landing Site Workhopmentioning
confidence: 99%
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“…Golombek et al, 2013 ;Wigton et al, 2014 ), with a fine regolith layer (e.g. Ruff and Christensen, 2002 ;Nowicki and Christensen, 2007 ;Warner et al, 2014 ) typically 10 m thick (Golombek et al, 2013 ). The equatorial location reduces the chance of encountering ices in the regolith (e.g Boynton et al, 2002 ).…”
Section: Measurement Locationsmentioning
confidence: 99%
“…Kieffer et al, 1977 ;Mellon et al, 2000 ;Christensen et al, 2001 ). This is achieved by using the known association of thermal inertia with regolith particle size, both of which correlate strongly with thermal conductivity at given temperatures and pressures (Nowicki and Christensen, 2007 ; While Martian thermal properties show some temperature dependence, these are mostly apparent over the large diurnal temperature variation. The focus here on seasonal average thermal properties should mitigate the influence of perturbing effects due to the temperature variation.…”
Section: Thermal Conductivity and Capacitymentioning
confidence: 99%