Visible/near-infrared spectrogoniometric observations and modeling of dust-coated rocks

Johnson, J. R.; Grundy, W. M.; Shepard, Michael K.

doi:10.1016/j.icarus.2004.05.013

Cited by 24 publications

(24 citation statements)

References 34 publications

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“…If this model is valid, the coatings must be extremely thin, probably on the order of a few to less than 10 microns, comparable to only a few times the average grain size of typical martian dust particles. These kinds of spectral effects from thin bright dust coatings over lower albedo rocky or sandy substrates on Mars have also been inferred from previous orbital and Pathfinder remote sensing observations (e.g., Fischer and Pieters, 1993;Johnson et al, 1999;Bell et al, 2000) and have been directly observed and modeled in laboratory simulations of Mars-like dust covering/coating Mars-like basaltic rocks and other substrates (e.g., Johnson and Grundy, 2001;Johnson et al, 2004Johnson et al, , 2006Kinch et al, 2006; see also Chapter 19 by Johnson et al).…”

Section: "Gray" Rock Grindings and "White" Rock Coatingssupporting

confidence: 66%

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Bell

Calvin²,

Farrand³

et al. 2008

The Martian Surface

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Multispectral imaging from the Panoramic Camera (Pancam) instruments on the Mars Exploration Rovers Spirit and Opportunity has provided important new insights about the geology and geologic history of the rover landing sites and traverse locations in Gusev crater and Meridiani Planum. Pancam observations from near-UV to near-IR wavelengths provide limited compositional and mineralogic constraints on the presence abundance, and physical properties of ferric-and ferrous-iron bearing minerals in rocks, soils, and dust at both sites. High resolution and stereo morphologic observations have also helped to infer some aspects of the composition of these materials at both sites. Perhaps most importantly, Pancam observations were often efficiently and effectively used to discover and select the relatively small number of places where in situ measurements were performed by the rover instruments, thus supporting and enabling the much more quantitative mineralogic discoveries made using elemental chemistry and mineralogy data. This chapter summarizes the major compositionally-and mineralogicallyrelevant results at Gusev and Meridiani derived from Pancam observations. Classes of materials encountered in Gusev crater include outcrop rocks, float rocks, cobbles, clasts, soils, dust, rock grindings, rock coatings, windblown drift deposits, and exhumed whitish/yellowish salty soils. Materials studied in Meridiani Planum include sedimentary outcrop rocks, rock rinds, fracture fills, hematite spherules, cobbles, rock fragments, meteorites, soils, and windblown drift deposits. This chapter also previews the results of a number of coordinated observations between Pancam and other rover-based and Mars-orbital instruments that were designed to provide complementary new information and constraints on the mineralogy and physical properties of martian surface materials. 13

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Section: "Gray" Rock Grindings and "White" Rock Coatingssupporting

confidence: 66%

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Bell

Calvin²,

Farrand³

et al. 2008

The Martian Surface

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“…Aeolian dust is a prominent component of the Martian surface environment. The properties and dynamics of this dust attracts attention for several reasons: The presence of airborne dust has implications for atmospheric heating rates and thereby atmospheric dynamics [e.g., Murphy et al , 1993; Pollack et al , 1995]; active deposition and erosion of dust contributes to the visual and infrared appearance of the planetary surface [e.g., Pollack and Sagan , 1967; Lee et al , 1982; Thomas et al , 1999; Edgett and Malin , 2001; Edgett , 2002] and so the presence of surficial dust deposits must be taken into account for correct interpretation of data from both remote‐sensing and in‐situ observations of surface materials [e.g., Johnson et al , 2003, 2004]. Finally, dust deposition represents a threat to the survival of mechanisms and instrumentation operating on Mars through obscuration of solar panels [ Landis , 1996; Landis and Jenkins , 2000] and possibly contamination of moving parts and optics.…”

Section: Introductionmentioning

confidence: 99%

Dust deposition on the Mars Exploration Rover Panoramic Camera (Pancam) calibration targets

Kinch¹,

Sohl-Dickstein²,

Bell³

et al. 2007

J. Geophys. Res.

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[1] The Panoramic Camera (Pancam) on the Mars Exploration Rover mission has acquired in excess of 20,000 images of the Pancam calibration targets on the rovers. Analysis of this data set allows estimates of the rate of deposition and removal of aeolian dust on both rovers. During the first 150-170 sols there was gradual dust accumulation on the rovers but no evidence for dust removal. After that time there is ample evidence for both dust removal and dust deposition on both rover decks. We analyze data from early in both rover missions using a diffusive reflectance mixing model. Assuming a dust settling rate proportional to the atmospheric optical depth, we derive spectra of optically thick layers of airfall dust that are consistent with spectra from dusty regions on the Martian surface. Airfall dust reflectance at the Opportunity site appears greater than at the Spirit site, consistent with other observations. We estimate the optical depth of dust deposited on the Spirit calibration target by sol 150 to be 0.44 ± 0.13. For Opportunity the value was 0.39 ± 0.12. Assuming 80% pore space, we estimate that the dust layer grew at a rate of one grain diameter per $100 sols on the Spirit calibration target. On Opportunity the rate was one grain diameter per $125 sols. These numbers are consistent with dust deposition rates observed by Mars Pathfinder taking into account the lower atmospheric dust optical depth during the Mars Pathfinder mission.

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“…The present study reveals that, for better spectral characterization, recognition and discrimination of lithological units are necessary, which is possible from remotely sensed data collected in the field. The spectral regions where fresh and weathered surfaces show spectral fluctuations can be used to better characterize and discriminate lithological units [48,54]. This study demonstrates the spectral differences between weathered and fresh surfaces caused by mineralogical changes induced by weathering.…”

Section: Discussionmentioning

confidence: 73%

“…A broad and symmetric band that appears in the 1000 nm region could be caused by Fe 2+ -Fe 3+ crystal field transitions on the weathered and fresh surfaces [48]. Broad hydroxyl bands are present near 1400 nm and 1900 nm.…”

Section: Spectral Features Of Dioritementioning

confidence: 96%

Spectral properties of weathered and fresh rock surfaces in the Xiemisitai metallogenic belt, NW Xinjiang, China

Zhou

Wang

2017

Open Geosciences

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Surfaces weathering of rocks in which mineral materials may be similar to or quite different from the minerals in the underlying parent rock completely control the reflectance spectra of the terrain. Our study of typical weathered and fresh rock samples from the Xiemisitai metallogenic belt, Western Junggar region, Xinjiang, found that weathering results in the formation of new materials that cause differences in the spectral features of fresh and weathered rock surfaces. Alterations induce variations in spectrum brightness, presence and intensity of characteristic absorption features, and spectral slope. Spectral differences between weathered and fresh rock surfaces are small for rhyolite, granite, and tuffaceous sandstone, but large for andesite, basalt, and diorite. Spectral changes in the 350-1000 nm wavelength region are attributed to alteration of iron oxides by atmospheric processes or secondary alteration of iron-rich minerals. Spectral features between 1000-2500 nm are caused by O-H vibrations, with features at 2200-2500 nm solely attributed to hydroxyl groups. The strongest Al-OH bands appear near 2200 nm, while Mg-OH bands are found near 2300 nm and 2350 nm. Results from this study can be used to better characterize and discriminate lithological units and potential mineral zones using hyperspectral and multispectral remote sensing techniques.

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Visible/near-infrared spectrogoniometric observations and modeling of dust-coated rocks

Cited by 24 publications

References 34 publications

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Mars Exploration Rover Pancam multispectral imaging of rocks, soils, and dust at Gusev crater and Meridiani Planum

Dust deposition on the Mars Exploration Rover Panoramic Camera (Pancam) calibration targets

Spectral properties of weathered and fresh rock surfaces in the Xiemisitai metallogenic belt, NW Xinjiang, China

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