Thermal imaging of the surface of Mars

Selivanov, A. S.; Naraeva, M. K.; Panfilov, A. S.; Gektin, Yu. M.; Kharlamov, V. D.; Romanov, A. V.; Fomin, D. A.; Miroshnichenko, Y. Y.

doi:10.1038/341593a0

Cited by 27 publications

(7 citation statements)

References 6 publications

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“…We use this term because the outcrop materials exhibit the variety of properties common to terrestrial layered rock outcrops. Thermophysical properties estimated from Phobos 2 Termoskan and TES observations suggest that larger exposures, such as the light-toned intracrater outcrops of Terra Meridiani and the layered material in the Valles Marineris, have an elevated thermal inertia consistent with the presence of unconsolidated coarse-grained material, but none of these observations have spatial resolution sufficient to see the thermal signature of solid rock if the rock is not cleanly exposed at the scales of 2 to 5 km (94,95). 43.…”

Section: Valles Imentioning

confidence: 94%

Sedimentary Rocks of Early Mars

Malin

Edgett

2000

Science

776

730

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Layered and massive outcrops on Mars, some as thick as 4 kilometers, display the geomorphic attributes and stratigraphic relations of sedimentary rock. Repeated beds in some locations imply a dynamic depositional environment during early martian history. Subaerial (such as eolian, impact, and volcaniclastic) and subaqueous processes may have contributed to the formation of the layers. Affinity for impact craters suggests dominance of lacustrine deposition; alternatively, the materials were deposited in a dry, subaerial setting in which atmospheric density, and variations thereof mimic a subaqueous depositional environment. The source regions and transport paths for the materials are not preserved.

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Section: Valles Imentioning

confidence: 94%

Sedimentary Rocks of Early Mars

Malin

Edgett

2000

Science

776

730

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“…The thermal emission of the martian surface has been investigated with a number of flyby and orbital instruments, including Mariner 6/7 Infrared Spectrometers (IRS), Mariner 9 Mars Infrared Spectrometer (IRIS), Viking Infrared Thermal Mapper (IRTM), Phobos 2 Thermoscan, Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES), and Mars Odyssey Thermal Imaging System (THEMIS) (Hanel et al, 1972;Herr et al, 1972;Kieffer et al, 1977;Selivanov et al, 1989;Christensen et al, 2001;Christensen et al, 2004). The measured thermal radiance can be used to infer the thermophysical properties of the upper surface layer by modeling the diurnal temperature response of the surface.…”

Section: Thermal Inertia Background and Derivationmentioning

confidence: 99%

The geology of the Viking Lander 2 site revisited

Thomson

Schultz

2007

Icarus

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“…Termoskan was a two-channel optical-mechanical scanning radiometer with one visible channel (0.5-1.0 mm) and one thermal infrared channel (8.5-12.0 ram) [Selivanov et al, 1989; Tcrmoskan's resolution per pixel at nadir was 1.8 km for three of the four panoramas acquired and 300 m for the remaining panorama [Selivanov et al, 1989;Murray et al, 1991]. These resolutions per pixel are much better than those obtained by the Viking infrared thermal mapper (IRTM) (approximately 5 to 170 km, with only a small fraction of the data near 5 km/pixel).…”

Section: Gel'hod Of Obsf_rvation and Data Analysismentioning

confidence: 99%

Thermally distinct ejecta blankets from Martian craters

Betts¹,

Murray²

1993

J. Geophys. Res.

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Utilizing the Termoskan data set of the Phobos '88 mission we have recognized a new feature on Mars: ejecta blanket distinct in the thermal infrared (EDITH). Virtually all of the more than 100 features discovered in the Termoskan data are located on the plains near Valles Marineris. EDITHs have a startlingly clear dependence upon terrains of Hesperian age, implying a spatial or temporal dependence on Hesperian terrains. Almost no thermally distinct ejecta blankets are associated with any of the thousands of craters within the data set that occur on the older Noachian units. EDITHs also do not appear on the portions of the younger Tharsis Amazonian units seen in the data. The Hesperian terrain dependence cannot be explained by either atmospheric or impactor variations; Noachian and Hesperian terrains must have experienced identical atmospheric and impactor conditions during Hesperian times. Thermally distinct ejecta blankets therefore reflect target material differences and/or secondary modification processes. Not all lobate ejecta blankets are thermally distinct, but all EDITHs correlated with visibly discernible ejecta blankets are associated with lobate ejecta blankets. The boundaries of the thermally distinct areas usually follow closely the termini of the fluidized lobate ejecta blankets, even when the ejecta blankets show a high degree of sinuosity. Thus, the thermally distinct nature of EDITHs must be due to the primary ejecta formation process. The coupling of these thermal anomalies to morphology is unlike most sharp Martian inertia variations which are decoupled from observed surface morphology. Some thermally distinct ejecta blankets occur near otherwise similar craters that do not have thermally distinct ejecta blankets. Thus, wind patterns or locally available aeolian material cannot provide a single overall explanation for the observed variations. We compiled a data base of 110 EDITH and non-EDITH craters ranging in diameter from 4.2 km to 90.6 km. There are almost no correlations within the data base other than occurrence on Hesperian terrains. We postulate that most of the observed EDITHs are due to excavation of thermally distinctive Noachian age material from beneath a relatively thin layer of younger, more consolidated Hesperian volcanic material. The plausibility of this theory is supported by much geological evidence for relatively thin near-surface Hesperian deposits overlying massive Noachian megabreccias on the EDITH-rich plains units. We suggest that absence of thermally distinct ejecta blankets on Noachian and Amazonian terrains is due to absences of distinctive near-surface layering. Thermally distinct ejecta blankets are excellent locations for future landers and remote sensing •cause of relatively dust free surface exposures of material excavated from depth. . Laboratory experiments that vary atmospheric pressure and particle size have also reproduced some lobate crater morphologies Gault, 1979, 1984]. One of our motivations in studying Martian thermally distinct ejecta blankets in d...

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Thermal imaging of the surface of Mars

Cited by 27 publications

References 6 publications

Sedimentary Rocks of Early Mars

Sedimentary Rocks of Early Mars

The geology of the Viking Lander 2 site revisited

Thermally distinct ejecta blankets from Martian craters

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