Mineralogical constraints on the high-silica martian surface component observed by TES

Michalski, J.; Kraft, Michaël; Sharp, T. G.; Williams, Lynda B.; Christensen, P. R.

doi:10.1016/j.icarus.2004.10.022

Cited by 137 publications

(147 citation statements)

References 77 publications

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“…Thermal infrared data acquired from Thermal Emission Spectrometer (TES) indicate a relatively silica-enriched surface (surface type II) compared to the typical basalt (Surface type I) of the southern highlands [Christensen et al, 2001]. Therefore, the surface of the lowlands was initially interpreted to be andesitic in composition [Bandfield et al, 2000] but later reinterpreted to represent altered terrains [e.g., Wyatt and McSween, 2002;Kraft et al, 2003;Michalski et al, 2005]. Gamma Ray Spectrometer data do not show enhancement of Si in the bulk rock [Karunatillake et al, 2006;Boynton et al, 2007], thus favoring the interpretation that spectral differences may be explained by the presence of a thin silica-enriched coating or rind [e.g., Kraft et al, 2003].…”

Section: History and Composition Of The Northern Lowlandsmentioning

confidence: 99%

The stratigraphy and history of Mars' northern lowlands through mineralogy of impact craters: A comprehensive survey

et al. 2017

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The basin‐filling materials of the northern lowlands, which cover approximately one third of Mars' surface, record the long‐term evolution of Mars' geology and climate. The buried stratigraphy was inferred through analyses of impact crater mineralogy, detected using data acquired by the Compact Reconnaissance Imaging Spectrometer for Mars. Examining 1045 impact craters across the northern lowlands, we find widespread olivine and pyroxene and diverse hydrated/hydroxylated minerals, including Fe/Mg smectite, chlorite, prehnite, and hydrated silica. The distribution of mafic minerals is consistent with infilling volcanic materials across the entire lowlands (~1–4 × 107 km3), indicating a significant volume of volatile release by volcanic outgassing. Hydrated/hydroxylated minerals are detected more frequently in large craters, consistent with the scenario that the hydrated minerals are being excavated from deep basement rocks, beneath 1–2 km thick mafic lava flows or volcaniclastic materials. The prevalences of different types of hydrated minerals are similar to statistics from the southern highlands. No evidence of concentrated salt deposits has been found, which would indicate a long‐lived global ocean. We also find significant geographical variations of local mineralogy and stratigraphy in different basins (geological provinces), independent of dust cover. For example, many hydrated and mafic minerals are newly discovered within the polar Scandia region (>60°N), and Chryse Planitia has more mafic mineral detections than other basins, possibly due to a previously unrecognized volcanic source.

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Section: History and Composition Of The Northern Lowlandsmentioning

confidence: 99%

The stratigraphy and history of Mars' northern lowlands through mineralogy of impact craters: A comprehensive survey

et al. 2017

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“…The group ''high-silica phases" includes silica glass, opal, zeolite minerals, and phyllosilicate minerals. These phases cannot be reliably distinguished from one another in TES deconvolution models (e.g., Bandfield, 2002;Michalski et al, 2003;Michalski et al, 2005), particularly if individual constituents are present in low abundance.…”

Section: Quantitative Mineralogical Analysismentioning

confidence: 99%

Mineralogical characterization of Mars Science Laboratory candidate landing sites from THEMIS and TES data

Rogers

2009

Icarus

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“…The MGS TES team assumed that the latter glass component was a primary volcanic glass consistent with basaltic andesites (Bandfield et al, 2000). Many attempts have been made to derive alternative composition for the enigmatic ST2 spectral endmember (Wyatt and McSween, 2002;Minitti et al, 2002Minitti et al, , 2007bKraft et al, 2003;Morris et al, 2003;Michalski et al, 2005Michalski et al, , 2006. The composition of ST2 areas still remains a subject of considerable debate (Wyatt, 2007), but chemically altered basalts…”

Section: +mentioning

confidence: 99%

“…It has been shown by several researchers that SiO 2 -rich component is still required for the successful deconvolution of the ST2 spectra but may be just a secondary product (e.g., silica-rich amorphous coatings), rather than a primary volcanic glass (Kraft et al, 2003;Morris et al, 2003;Michalski et al, 2005Michalski et al, , 2006Minitti et al, 2007b;Ruff and Christensen, 2007). The recent orbital detection of opaline silica by CRISM ) and the recent discovery of opal in Gusev crater by the Spirit rover (Squires et al 2008) show that amorphous silica indeed is not an uncommon weathering product on Mars.…”

Section: +mentioning

confidence: 99%

Spectral properties of simulated impact glasses produced from martian soil analogue JSC Mars-1

Moroz

Basilevsky

Hiroi

et al. 2009

Icarus

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To simulate the formation of impact glasses on Mars, an analogue of Martian bright soil (altered volcanic soil JSC Mars-1) was melted at relevant oxygen fugacities using a pulsed laser and a resistance furnace. Reduction of Fe 3+ to Fe 2+ and in some cases formation of nanophase Fe spatial resolution and wavelength coverage may detect impact glasses at certain locations, e.g., in the vicinity of fresh impact craters. Such dark materials are usually interpreted as accumulations of mafic volcanic sand, but the possibility of an impact melt origin of such materials also should be considered. In addition, our data suggest that high contents of feldspars or zeolites are not necessary to produce the transparency feature at 12.1 µm typical of Martian dust spectra.

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Mineralogical constraints on the high-silica martian surface component observed by TES

Cited by 137 publications

References 77 publications

The stratigraphy and history of Mars' northern lowlands through mineralogy of impact craters: A comprehensive survey

The stratigraphy and history of Mars' northern lowlands through mineralogy of impact craters: A comprehensive survey

Mineralogical characterization of Mars Science Laboratory candidate landing sites from THEMIS and TES data

Spectral properties of simulated impact glasses produced from martian soil analogue JSC Mars-1

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