TES premapping data: Slab ice and snow flurries in the Martian north polar night

Titus, T. N.; Kieffer, H. H.; Mullins, K. F.; Christensen, P. R.

doi:10.1029/2000je001284

Cited by 60 publications

(68 citation statements)

References 26 publications

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“…Eluszkiewicz [1993] predicted the presence of both nonporous (slab-like) CO 2 ice and more porous, fluffy frost, a prediction confirmed by subsequent analyses [Kieffer et al, 2000;Titus et al, 2001] (for completeness, we note that according to Langevin et al [2006], dust coating can also mimic the slab ice behavior). A fluffy texture can be distinguished from a slab layer by the shape of the 25-mm band of solid CO 2 [Hansen, 1997] seen in the TES spectra, with large band depth BD 25 indicative of high porosity.…”

Section: Tes Datamentioning

confidence: 66%

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Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

Eluszkiewicz¹,

Moncet²,

Shephard³

et al. 2008

J. Geophys. Res.

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[1] Retrievals of atmospheric temperatures, surface emissivities, and dust opacities in the Mars polar regions from the Thermal Emission Spectrometer (TES) spectra are presented. The retrievals correspond to two types of spectra, characterized by small and large band depths BD 25 in the 25-mm band of solid CO 2 . These two types of spectra have previously been identified with locations covered by slab ice and fluffy CO 2 frost, respectively. Above the first atmospheric scale height, there is a correlation between the degree of saturation in the retrieved atmospheric temperatures and the two types of surface, with the high BD 25 spectra (''cold spots'') showing larger supersaturations around 1 mbar. This supports the hypothesis that cold spots correspond to locations with potential or actual atmospheric precipitation. Furthermore, the retrieved temperature profiles exhibit a warming above 1 mbar (15 km), which appears real even when the limited number of independent pieces of information from the measurement ($3) and coarse vertical resolution of the TES instrument above 15 km are considered. The spectral shape of the retrieved surface emissivities in the cold spot locations is consistent with modeling results attributing high BD 25 to porosity. For the low BD 25 spectra, the retrieved emissivities are spectrally flat but significantly less than unity (0.8-0.9). The cause of these spectrally uniform deviations from blackbody behavior (which are not supported by modeling) remains to be investigated, with a noticeable reduction in the deviation from the blackbody behavior achieved through a zero-radiance-level correction to the TES spectra available from the Planetary Data System.

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Section: Tes Datamentioning

confidence: 66%

“…Cold spots have been identified in the TES spectra of the polar regions [Titus et al, 2001;Eluszkiewicz et al, 2005a]. These locations form one of the foci of the retrieval work presented herein.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

Eluszkiewicz¹,

Moncet²,

Shephard³

et al. 2008

J. Geophys. Res.

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“…TES observations of the south polar region during the aerobraking phase (southern summer) revealed an unexpected large range of CO 2 albedo (Kieffer et al 2000) (termed herein Paper I) and observations of the northern winter cap showed that CO 2 condensation occurred in three forms, including a slab-ice form thought to be the cause of the low-albedo CO 2 deposits (Titus et al 2001) (termed herein Paper II). The brightness variations of CO 2 and H 2 O seasonal frosts are a major aspect of this current paper.…”

Section: Introductionmentioning

confidence: 98%

TES Mapping of Mars' North Seasonal Cap

Kieffer

Titus

2001

Icarus

134

150

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“…Principal component analysis of representative data indicates that there are three primary forms of condensing CO2: fine-grained crystals with a broad low spectral emissivity at 25 /xm (the "U" member), coarser-grained crystals with a somewhat weaker and sharper emissivity depression (the "V" member), and slab ice with a spectrum close to a blackbody (the "B" member) [Titus et al, 2001].…”

Section: Condensation Season In the Northmentioning

confidence: 99%

Mars Global Surveyor Thermal Emission Spectrometer experiment: Investigation description and surface science results

et al. 2001

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Abstract. The Thermal Emission Spectrometer (TES) investigation on Mars GlobalThe TES data are calibrated to a 1-o-precision of 2.5 -6 X 10 -8 W cm -2 sr-1/cm -•, 1.6 x 10 -6 W cm -2 sr -•, and -0.5 K in the spectrometer, visible/near-IR bolometer, and IR bolometer, respectively_. These instrument subsections are calibrated to an absolute accuracy of-4 x 10 -8 W cm -2 sr-•/cm -• (0.5 K at 280 K), 1-2%, and -1-2 K, respectively. Global mapping of surface mineralogy at a spatial resolution of 3 km has shown the following: (1) The mineralogic composition of dark regions varies from basaltic, primarily plagioclase feldspar and clinopyroxene, in the ancient, southern highlands to andesitic, dominated by plagioclase feldspar and volcanic glass, in the younger northern plains. (2) Aqueous mineralization has produced gray, crystalline hematite in limited regions under ambient or hydrothermal conditions; these deposits are interpreted to be in-place sedimentary rock formations and indicate that liquid water was stable near the surface for a long period of time. (3) There is no evidence for large-scale (tens of kilometers) occurrences of moderate-grained (>50-•m) carbonates exposed at the surface at a detection limit of -10%. (4) Unweathered volcanic minerals dominate the spectral properties of dark regions, and weathering products, such as clays, have not been observed anywhere above a detection limit of -10%; this lack of evidence for chemical weathering indicates a geologic history dominated by a cold, dry climate in which mechanical, rather than chemical, weathering was the significant form of erosion and sediment production. (5) There is no conclusive evidence for sulfate minerals at a detection limit of -15%. The polar region has been studied with the following major conclusions: (1) Condensed CO2 has three distinct end-members, from fine-grained crystals to slab ice. (2) The growth and retreat of the polar caps observed by MGS is virtually the same as observed by Viking 12 Martian years ago. (3) Unique regions have been identified that appear to differ primarily in the grain size of CO2; one south polar region appears to remain as black slab CO2 ice throughout its sublimation. (4) Regional atmospheric dust is common in localized and regional dust storms around the margin and interior of the southern cap. Analysis of the thermophysical properties of the surface shows that (1) the spatial pattern of albedo has changed since Viking observations, (2) a unique cluster of surface materials with intermediate inertia and albedo occurs that is distinct from the previously identified lowinertia/bright and high-inertia/dark surfaces, and (3) localized patches of high-inertia material have been found in topographic lows and may have been formed by a unique set of aeolian, fluvial, or erosional processes or may be exposed bedrock.• •Raytheon Santa Barbara Remote Sensing, Goleta, California. IntroductionThe Thermal Emission Spectrometer (TES) experiment is designed to address a wide range of science objectives, including the de...

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TES premapping data: Slab ice and snow flurries in the Martian north polar night

Cited by 60 publications

References 26 publications

Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

TES Mapping of Mars' North Seasonal Cap

Mars Global Surveyor Thermal Emission Spectrometer experiment: Investigation description and surface science results

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