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

Mellon, M. T.

doi:10.1006/icar.2000.6503

Cited by 491 publications

(586 citation statements)

References 47 publications

(92 reference statements)

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“…We calculate that rock surface temperature varies on this day from 186 to 192 K ( NATURE COMMUNICATIONS | DOI: 10.1038/ncomms7712 ARTICLE temperature range is consistent with THEMIS data, which shows decreasing range in temperature with increasing thermal inertia 41 . Bedrock has a higher thermal conductivity than unconsolidated sediment, resulting in four to five times higher thermal inertia 42,43 .…”

Section: Resultssupporting

confidence: 84%

Cracks in Martian boulders exhibit preferred orientations that point to solar-induced thermal stress

et al. 2015

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The origins of fractures in Martian boulders are unknown. Here, using Mars Exploration Rover 3D data products, we obtain orientation measurements for 1,857 cracks visible in 1,573 rocks along the Spirit traverse and find that Mars rock cracks are oriented in statistically preferred directions similar to those compiled herein for Earth rock cracks found in mid-latitude deserts. We suggest that Martian directional cracking occurs due to the preferential propagation of microfractures favourably oriented with respect to repeating geometries of diurnal peaks in sun-induced thermal stresses. A numerical model modified here with Mars parameters supports this hypothesis both with respect to the overall magnitude of stresses as well as to the times of day at which the stresses peak. These data provide the first direct field and numerical evidence that insolation-related thermal stress potentially plays a principle role in cracking rocks on portions of the Martian surface.

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Section: Resultssupporting

confidence: 84%

Cracks in Martian boulders exhibit preferred orientations that point to solar-induced thermal stress

et al. 2015

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“…Thermal inertias of the Viking 1 and 2 and Mars Pathfinder (MPF) landing sites as derived from TES data were discussed by Mellon et al [2000]. Here we will expand on that discussion in the context of using the in situ observations at these sites to help interpret observations at locations for which we have no ground truth observations.…”

Section: Properties Of Viking and Pathfinder Landing Sitesmentioning

confidence: 97%

High‐resolution thermal inertia mapping of Mars: Sites of exobiological interest

Jakosky¹,

Mellon²

2001

J. Geophys. Res.

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Abstract. We have mapped thermal inertia at high resolution for selected regions of Mars that are of potential biological relevance, using observations made by the Mars Global Surveyor Thermal Emission Spectrometer. Thermal inertia is a direct indicator of physical properties of the surface at the decimeter-to-meter scale. Our goal is to understand the geological processes by which the sites formed and their subsequent evolution, their current state, and their safety and science potential as landing sites for future lander, rover, and sample-return spacecraft missions. The thermal inertia values at -3-km scale for the sites considered span the entire range of values measured at Mars; thermal inertias range from low values indicative of substantial aeolian mantling up to high values suggesting surfaces covered predominantly with bedrock, exposed rocks or blocks, or wellindurated crusts. The highest thermal inertias correlate strongly with local morphology, while areas with intermediate and low thermal inertias generally show no such correlation. This suggests that selection of future landing sites will be plagued by a choice of a well-mantled site that is safe but less interesting scientifically versus an unmantied site that is more interesting scientifically but less safe.

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“…This model assumes a circular symmetry around the SEP. From thermal emission observations and models (Mellon et al 2000), it is known that the maximum temperature occurs after local noon. However, due to our relatively low spatial resolution (half of the planetary disk at 230-GHz), we only need to obtain a good approximation of the MCD disk-averaged surface temperature.…”

Section: Surface Parametersmentioning

confidence: 99%

Vertical temperature profile and mesospheric winds retrieval on Mars from CO millimeter observations

Cavalié

Billebaud

Encrenaz

et al. 2008

A&A

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Aims.We have recorded high spectral resolution spectra and derived precise atmospheric temperature profiles and wind velocities in the atmosphere of Mars. We have compared observations of the planetary mean thermal profile and mesospheric wind velocities on the disk, obtained with our millimetric observations of CO rotational lines, to predictions from the Laboratoire de Météorologie Dynamique (LMD) Mars General Circulation Model, as provided through the Mars Climate Database (MCD) numerical tool. Methods. We observed the atmosphere of Mars at CO(1−0) and CO(2−1) wavelengths with the IRAM 30-m antenna in June 2001 and November 2005. We retrieved the mean thermal profile of the planet from high and low spectral resolution data with an inversion method detailed here. High spectral resolution spectra were used to derive mesospheric wind velocities on the planetary disk. We also report here the use of 13 CO(2−1) line core shifts to measure wind velocities at 40 km.

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

Cited by 491 publications

References 47 publications

Cracks in Martian boulders exhibit preferred orientations that point to solar-induced thermal stress

Cracks in Martian boulders exhibit preferred orientations that point to solar-induced thermal stress

High‐resolution thermal inertia mapping of Mars: Sites of exobiological interest

Vertical temperature profile and mesospheric winds retrieval on Mars from CO millimeter observations

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