Calcium carbonate and sulfate of possible extraterrestrial origin in the EETA 79001 meteorite

Gooding, J. L.; Wentworth, S. J.; Zolensky, M. E.

doi:10.1016/0016-7037(88)90361-4

Cited by 138 publications

(125 citation statements)

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“…Similarly, Treiman et al (1993) described smectite in Lafayette. Carbonate and sulphate minerals were first identified within the EETA79001 martian meteorite (Gooding et al, 1988) although their presence had earlier been inferred through pyrolysis or stepped combustion experiments (Carr et al, 1985;Gooding and Muenow, 1986). Subsequent studies (summarised in Table I) have enabled the mineralogical and stable isotope characteristics to be understood in more detail.…”

Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

“…The shergottite EETA79001 contains calcite and sulphate but located within druse cavities in the glassy parts of that meteorite (Gooding et al, 1988). ALH84001 has the most abundant carbonate and the largest grains or "rosettes" (≤250 µm, Figure 1c, d).…”

Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

“…However, there is also evidence for an association with shock remobilisation, particularly in ALH84001 (e.g. Scott et al, 1997) and possibly EETA79001 (Gooding et al, 1988). It has also been suggested that hydrothermal processes (by which we mean fluid activity at relatively high temperatures >150 • C, compared to those of groundwater), may also have left traces within the meteorites (e.g.…”

Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

“…These signs include melt pockets, deformation features in the silicate minerals and the presence of maskelynite. Gooding et al (1988) suggested that the salts within the "lithology C" of EETA79001, which is largely composed of shock melt, might have been entrained from the martian surface into the parent rock during the impact melting event. Evaporite sediments might have been assimilated into the cooling Nakhla parent lava (Bridges and Grady, 1999), although subsequently a direct evaporation model, described in the previous section, was found to be more consistent with the mineralogical features in the 3 nakhlites (Bridges and Grady, 2000).…”

Section: High Temperature: Shock Remobilisation Andmentioning

confidence: 99%

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Bridges

Catling

Saxton

et al. 2001

Space Science Reviews

215

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Abstract. The SNC (Shergotty-Nakhla-Chassigny) meteorites have recorded interactions between martian crustal fluids and the parent igneous rocks. The resultant secondary minerals -which comprise up to ~ 1 vol.% of the meteorites -provide information about the timing and nature of hydrous activity and atmospheric processes on Mars. We suggest that the most plausible models for secondary mineral formation involve the evaporation of low temperature (25-150 o C) brines. This is consistent with the simple mineralogy of these assemblages -Fe-Mg-Ca carbonates, anhydrite, gypsum, halite, clays -and the chemical fractionation of Ca-to Mg-rich carbonate in ALH84001 'rosettes'. Longer-lived, and higher temperature, hydrothermal systems would have caused more silicate alteration than is seen and probably more complex mineral assemblages. Experimental and phase equilibria data on carbonate compositions similar to those present in the SNCs imply low temperatures of formation with cooling taking place over a short period of time (e.g. days). The ALH84001 carbonate also probably shows the effects of partial vapourisation and dehydration related to an impact event postdating the initial precipitation. This shock event may have led to the formation of sulphide and some magnetite in the Fe-rich outer parts of the rosettes.Radiometric dating (K-Ar, Rb-Sr) of the secondary mineral assemblages in one of the nakhlites (Lafayette) suggests that they formed between 0 and 670 Ma, and certainly long after the crystallisation of the host igneous rocks. Crystallisation of ALH84001 carbonate took place 0.5 Ga after the parent rock. These age ranges and the other research on these assemblages suggest that environmental conditions conducive to near-surface liquid water have been present on Mars periodically over the last ~1 Ga. This fluid activity cannot have been continuous over geological time because in that case much more silicate alteration would have taken place in the meteorite parent rocks and the soluble salts would probably not have been preserved.The secondary minerals could have been precipitated from brines with seawater-like composition, high bicarbonate contents and a weakly acidic nature. The co-existence of siderite (Fe-carbonate) and clays in the nakhlites suggests that the pCO 2 level in equilibrium with the parent brine may have been 50 mbar or more. The brines could have originated as flood waters which percolated through the top few hundred metres of the crust, releasing cations from the surrounding parent rocks. There is no spectroscopic or photographic evidence for extensive evaporite deposits on the current martian surface but some salt precipitation through solute concentration must have occurred as floodwaters associated with many of the martian channels ponded in low-lying areas. The high sulphur and chlorine concentrations of the martian soil have most likely resulted from aeolian redistribution of such aqueously-deposited salts and from reaction of the martian surface with volcanic acid volatiles. However, the SNC...

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Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

Section: Research On Secondary Minerals In Sncs and Models For Their mentioning

confidence: 99%

Section: High Temperature: Shock Remobilisation Andmentioning

confidence: 99%

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Bridges

Catling

Saxton

et al. 2001

Space Science Reviews

215

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“…Although this simi larity was prominently featured in their abstract, McKay et al [Mittlefehldt, 1994;Treiman, 1995]. However, the presence of grains of plagioclase glass and rare silica glass in fractures strongly suggests that these minerals were melted, dispersed in fractures, and cooled rapidly to glass [Scott et In ALH84001, as in EET79001 and Nakhla [Gooding et al, 1988[Gooding et al, , 1991, carbonates, sulfates, and other salts are mostly located in interstitial sites next to plagioclase or plagioclase glass and in fractures. It is plausible that these phases formed from fluids in interstitial pores that had been generated much earlier by the release of CO2 and other volatiles during the final stages of igneous crystallization.…”

Section: Carbonatementioning

confidence: 99%

Origin of carbonate‐magnetite‐sulfide assemblages in Martian meteorite ALH84001

Scott¹

1999

J. Geophys. Res.

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Orbital evidence for more widespread carbonate‐bearing rocks on Mars

et al. 2016

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Carbonates are key minerals for understanding ancient Martian environments because they are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for paleoatmospheric CO 2 . Previous remote sensing studies have identified mostly Mg-rich carbonates, both in Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older Fe-and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre basin and Valles Marineris, and in other isolated locations spread widely across the planet. In all cases they cooccur with or near phyllosilicates, and in Huygens basin specifically they occupy layered rocks exhumed from up to~5 km depth. We discuss factors that might explain their observed regional distribution, arguments for why carbonates may be even more widespread in Noachian materials than presently appreciated and what could be gained by targeting these carbonates for further study with future orbital or landed missions to Mars.

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Calcium carbonate and sulfate of possible extraterrestrial origin in the EETA 79001 meteorite

Cited by 138 publications

References 16 publications

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Origin of carbonate‐magnetite‐sulfide assemblages in Martian meteorite ALH84001

Orbital evidence for more widespread carbonate‐bearing rocks on Mars

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