Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Murchie, S. L.; Kirkland, L. E.; Erard, S.; Mustard, John F.; Robinson, M. S.

doi:10.1006/icar.2000.6446

Cited by 80 publications

(74 citation statements)

References 64 publications

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“…Similar to the Ytri eruptions, later eruptions from the troughs may have come from basalt at depth, which unable to mix with groundwater, may have yielded lava. Consistent with TES results for a basaltic composition for Hebes deposits (Christensen et al 1998) and near-infrared data from Phobos II that indicate a water-altered palagonite composition for the interior deposits (Murchie et al 2000), this phase may have included the eruption of basaltic lava beneath ponded ice, forming interior tuyas Fig. 14B).…”

Section: Malin and Edgettsupporting

confidence: 76%

“…Although many processes could form resistant rock, this origin could account for the selective occurrence of the caprock, as individual volcanoes form at different rates and times (ice levels may vary); some may not reach the meltwater boundary to form caprock. Supporting the interpretation of a sub-ice volcanic origin are the near-infrared spectral data from the ISM (imaging spectrometer for Mars) instrument on board Phobos 2 that indicate the interior mounds are highly water-altered palagonitic rocks (Murchie et al 2000). Although a tuya origin would require very thick ice sheets in the chasmata, it would be a much smaller water volume than that called for by a lacustrine origin, as water/ice levels would be below the putative-subaerial-lava caps of resistant material (Chapman and Tanaka 2001).…”

Section: Interior Deposits: Sub-ice Volcanoesmentioning

confidence: 99%

See 1 more Smart Citation

Related Magma–Ice Interactions: Possible Origins of Chasmata, Chaos, and Surface Materials in Xanthe, Margaritifer, and Meridiani Terrae, Mars

Chapman

Tanaka

2002

Icarus

124

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We examine here the close spatial and temporal associations among several unique features of Xanthe and Margaritifer Terrae, specifically the Valles Marineris troughs or chasmata and their interior deposits, chaotic terrain, the circum-Chryse outflow channels, and the subdued cratered material that covers Xanthe, Margaritifer, and Meridiani Terrae. Though previous hypotheses have attempted to explain the origin of individual features or subsets of these, we suggest that they may all be related. All of these features taken together present a consistent scenario that includes the processes of sub-ice volcanism and other magma/ice interactions, results of intrusive events during Late Noachian to Early Amazonian times. c 2002 Elsevier Science (USA)

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Section: Malin and Edgettsupporting

confidence: 76%

Section: Interior Deposits: Sub-ice Volcanoesmentioning

confidence: 99%

Related Magma–Ice Interactions: Possible Origins of Chasmata, Chaos, and Surface Materials in Xanthe, Margaritifer, and Meridiani Terrae, Mars

Chapman

Tanaka

2002

Icarus

124

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“…A wide variety of minerals has recently been detected on Mars' surface (e.g., Chevrier and Mathé, 2007 and references therein;Mustard et al 2008). Globally, however, most optical spectra of the Martian surface are roughly consistent with the mixing of bright red ferric oxide-bearing dust with dark gray sand containing mafic minerals (Singer and McCord, 1979;Murchie et al, 2000;). …”

Section: Implications For Mars and Conclusionmentioning

confidence: 85%

“…The bright regions on Mars are relatively homogeneous in the VNIR spectral range due to the high mobility of fine bright dust particles during dust storms, but show some spatial spectral variations (Murchie et al, 1993(Murchie et al, , 2000. Although impact glass fragments should contribute to these mobile fines (Schultz and Mustard 2004), their spectral signatures do not seem to be easily detectable in spectra of the soils.…”

Section: Implications For Mars and Conclusionmentioning

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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“…Absorption features in lander surface spectra (Bell et al, 2000) and magnetics experiments (Madsen et al, 1999) indicate the presence ofnanophase ferric oxides which suggest chemical weathering. Deposits of crystalline gray hematite recognized from MGS TES measurements in Sinus Meridani (Christensen et al, 2000b) and dispersed ferrihydrite in soils identified by orbital VISNIR spectroscopy (Murchie et al, 2000) are also attributedto aqueous processes. The response of Viking fines to heating (Biemann et al, 1977) and simulations of surface reflectance spectra suggest soil water contents of a few percent (Yen et al, 1998).…”

Section: Ar S Degassing H Ydrogeology An D Weathe Ringmentioning

confidence: 99%

The rocks of Mars, from far and near

McSween

2002

Meteorit & Planetary Scien

132

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Abstract-The age, structure, composition, and petrogenesis of the martian lithosphere have been constrained by spacecraft imagery and remote sensing. How well do martian meteorites conform to expectations derived from this geologic context? Both data sets indicate a thick, extensive igneous crust formed very early in the planet's history. The composition of the ancient crust is predominantly basaltic, possibly andesitic in part, with sediments derived from volcanic rocks. Later plume eruptions produced igneous centers like Tharsis, the composition of which cannot be determined because of spectral obscuration by dust. Martian meteorites (except Allan Hills 84001) are inferred to have come from volcanic flows in Tharsis or Elysium, and thus are not petrologically representative of most ofthe martian surface. Remote-sensing measurements cannot verify the fractional crystallization and assimilation that have been documented in meteorites, but subsurface magmatic processes are consistent with orbital imagery indicating thick crust and large, complex magma chambers beneath Tharsis volcanoes. Meteorite ejection ages are difficult to reconcile with plausible impact histories for Mars, and oversampling of young terrains suggests either that only coherent igneous rocks can survive the ejection process or that older surfaces cannot transmit the required shock waves. The mean density and moment of inertia calculated from spacecraft data are roughly consistent with the proportions and compositions ofmantle and core estimated from martian meteorites. Thermal models predicting the absence of crustal recycling, and the chronology of the planetary magnetic field agree with conclusions from radiogenic isotopes and paleomagnetism in martian meteorites. However, lack of vigorous mantle convection, as inferred from meteorite geochemistry, seems inconsistent with their derivation from the Tharsis or Elysium plumes. Geological and meteoritic data provide conflicting information on the planet's volatile inventory and degassing history, but are apparently being reconciled in favor of a periodically wet Mars. Spacecraft measurements suggesting that rocks have been chemically weathered and have interacted with recycled saline groundwater are confirmed by weathering products and stable isotope fractionations in martian meteorites.

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Near-Infrared Spectral Variations of Martian Surface Materials from ISM Imaging Spectrometer Data

Cited by 80 publications

References 64 publications

Related Magma–Ice Interactions: Possible Origins of Chasmata, Chaos, and Surface Materials in Xanthe, Margaritifer, and Meridiani Terrae, Mars

Related Magma–Ice Interactions: Possible Origins of Chasmata, Chaos, and Surface Materials in Xanthe, Margaritifer, and Meridiani Terrae, Mars

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

The rocks of Mars, from far and near

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