NanoSIMS analyses of apatite and melt inclusions in the GRV 020090 Martian meteorite: Hydrogen isotope evidence for recent past underground hydrothermal activity on Mars

Hu, Sen; Ye, Lin; Zhang, J.; Hao, Jialong; Feng, Liang; Xu, Lin; Yang, Wei; Yang, Jin‐Hui

doi:10.1016/j.gca.2014.05.008

Cited by 67 publications

(95 citation statements)

References 55 publications

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“…The high-temperature water source is interpreted to be the structural hydroxyl in the smectite in this mudstone, while the low-temperature water source may include later absorbed water (Mahaffy et al, 2015). This value (4600 ± 600h) is slightly lower than the surface water source inferred by Hu et al (2014), but higher than those reported by Usui et al (2015). It is possible that the martian surface contains heterogeneous water reservoirs due to temporal or spatial evolution of water on Mars.…”

Section: Source For the Volatile-rich End-membermentioning

confidence: 63%

“…Previously suggested sources include the martian atmosphere (Bogard and Johnson, 1983), soils (Rao et al, 1999), ground-water or ice (Hu et al, 2014;Usui et al, 2015), or aqueous-alteration products, as observed in nakhlites (Treiman et al, 1993). Bogard and Johnson (1983) suggested direct implantation of martian atmosphere (noble gases, N 2 , and CO 2 ) into meteorites.…”

Section: Source For the Volatile-rich End-membermentioning

confidence: 99%

“…The age-span of this water source is bracketed by the crystallization and ejection ages of the three meteorites . Interaction between martian rocks and ground water was also evoked by Hu et al (2014), based on zonation of water concentration and hydrogen isotopes in melt inclusions in olivines in shergottite GRV020090. This interaction occurred after the rock crystallized at 196 Ma (Jiang and Hsu, 2012), and the duration of the alteration is estimated to be from a few hundred to a few hundred thousand years based upon diffusion simulations (Hu et al, 2014).…”

Section: Introductionmentioning

confidence: 99%

“…Interaction between martian rocks and ground water was also evoked by Hu et al (2014), based on zonation of water concentration and hydrogen isotopes in melt inclusions in olivines in shergottite GRV020090. This interaction occurred after the rock crystallized at 196 Ma (Jiang and Hsu, 2012), and the duration of the alteration is estimated to be from a few hundred to a few hundred thousand years based upon diffusion simulations (Hu et al, 2014). However, the δD value of the ground water is inferred to be ∼6000h, substantially higher than the water sources suggested in Usui et al (2015).…”

Section: Introductionmentioning

confidence: 99%

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Evidence in Tissint for recent subsurface water on Mars

Chen

Liu

Guan

et al. 2015

Earth and Planetary Science Letters

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We report unambiguous chemical evidence for subsurface water activity in the martian crust at <600 Ma based on the data from Tissint, a fresh martian meteorite fall with minimal terrestrial weathering. The impact-melt pockets in Tissint contain abundant volatiles (H 2 O, CO 2 , F, and Cl), and their concentrations are positively correlated with each other. Higher H 2 O concentrations also accompany higher deuterium contents. These correlations suggest mixing between two volatile sources. The first source is H 2 O in the precursor basalt inherited from martian magma. Magmatic H 2 O in the basalt had low deuterium concentration and was likely stored in the nominally anhydrous minerals. This source contributed little CO 2 or halogens to the impact melts. The second source is inferred to be aqueous-alteration products introduced to the basalt by water activity after the basalt erupted. These alteration materials contributed more volatiles to the impact melts than the magmatic source, and had high deuterium abundance, reflecting isotope equilibrium with recent martian atmosphere. The water activities occurred beneath the martian surface after ∼600 Ma (crystallization age), but before ∼1 Ma (ejection age). The chemical and isotopic signatures of the alteration products in Tissint resemble previously known martian samples associated with old water activities on Mars, which can be traced back to ∼4.2 billion years ago (e.g., the mudstone at Gale Crater). This similarity in chemistry and the wide age-span indicate that such water activities were common on Mars throughout its history, which had the potential to form habitable environment. However, the rarity of the volatile-rich zone in Tissint suggests that Martian crustal aqueous processes, where they have occurred are generally limited in their extent of water-rock reaction.

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Section: Source For the Volatile-rich End-membermentioning

confidence: 63%

Section: Source For the Volatile-rich End-membermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Evidence in Tissint for recent subsurface water on Mars

Chen

Liu

Guan

et al. 2015

Earth and Planetary Science Letters

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“…6). This high δD is consistent with water from the martian surface which is readily exchanged with atmosphere (e.g., Jakosky and Jones, 1997;Greenwood et al, 2008;Hu et al, 2014;Usui et al 2015). In situ measurements by the Curiosity Rover suggest that martian surface and atmospheric waters have δD values in excess of 5000 ‰, and that water near the poles of Mars may have δD values as high as 7000 ‰ (Webster et al, 2013;Villanueva et al, 2014).…”

Section: The Volatile Inventory Of Tissint Shock-produced Glassmentioning

confidence: 64%

Martian low-temperature alteration materials in shock-melt pockets in Tissint: Constraints on their preservation in shergottite meteorites

Kuchka

Herd

Walton

et al. 2017

Geochimica et Cosmochimica Acta

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We apply an array of in situ analytical techniques, including electron and Raman microscopy, electron and ion probe microanalysis, and laser ablation mass spectrometry to the Tissint martian meteorite in order to find and elucidate a geochemical signature characteristic of low-temperature alteration at or near the martian surface. Tissint contains abundant shock-produced quench-crystallized melt pockets containing water in concentrations ranging from 73 to 1730 ppm; water content is positively correlated with Cl content. The isotopic composition of hydrogen in the shock-produced glass ranges from δD = 2559 to 4422 ‰. Water is derived from two distinct hydrogen reservoirs: the martian nearsurface (>500 ‰) and the martian mantle (-100 ‰). In one shock melt pocket comprising texturally homogeneous vesiculated glass, the concentration of H in the shock melt decreases while simultaneously becoming enriched in D, attributable to the preferential loss of H over D to the vesicle while the pocket was still molten. While igneous sulfides are pyrrhotite in composition (Fe 0.88-0.90 S), the iron to sulfur ratios of spherules in shock melt pockets are elevated, up to Fe 1.70 S, which we attribute to shock-oxidation of igneous pyrrhotite and the formation of hematite at high temperature. The D-and Cl-enrichment, and higher oxidation of the pockets (as indicated by hematite) support a scenario in which alteration products formed within fractures or void spaces within the rock; the signature of these alteration products is preserved within shock melt (now glass) which formed upon collapse of these fractures and voids during impact shock. Thermal modeling of Tissint shock melt pockets using the HEAT program demonstrates that the shock melt pockets with the greatest potential to preserve a signature of aqueous alteration are small, isolated from other regions of shock melt, vesicle-free, and glassy.3

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On the secular retention of ground water and ice on Mars

et al. 2017

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Tropical ground ice on Mars undergoes long‐term sublimation and likely exospheric escape. Without restriction of sublimation, the cryosphere would eventually breach, leading to massive loss of any underlying groundwater. We seek to understand the conditions under which the ground‐ice seal, groundwater, and subsurface habitability are preserved. Using multireservoir models for the evolution of deuterium‐to‐hydrogen ratios, we derive a median estimate of the Hesperian‐Amazonian H2O loss of 60 m (interquartile range 30–120 m) global equivalent layer (GEL), neglecting magmatic degassing. Most of the loss may have been early, with consequent low loss in the “modern” cold and dry climate. We modeled global H2O transport within Mars following an assumed abrupt transition to modern conditions at 3 Ga. Sublimation is retarded (in order of decreasing priority) by higher obliquity, smaller porosity, higher tortuosity, lower heat flow, and smaller pore radius. Higher obliquity reduces H2O loss by decreasing tropical surface temperatures and raising global atmospheric water vapor. Time‐variable obliquities do not overly influence outcomes as long as the total duration <30° obliquity is <1 Gyr, with no interval longer than a few hundred million years. Decreased solar luminosity or a thicker CO2 atmosphere can also retard loss of subsurface H2O, whereas lower atmospheric water vapor accelerates sublimation. If Mars' post‐Noachian crustal H2O inventory was a few hundred meters GEL or more, then the modest loss since then implies that the cryospheric seal has been maintained following top down freezing and that groundwater likely exists globally on Mars today.

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NanoSIMS analyses of apatite and melt inclusions in the GRV 020090 Martian meteorite: Hydrogen isotope evidence for recent past underground hydrothermal activity on Mars

Cited by 67 publications

References 55 publications

Evidence in Tissint for recent subsurface water on Mars

Evidence in Tissint for recent subsurface water on Mars

Martian low-temperature alteration materials in shock-melt pockets in Tissint: Constraints on their preservation in shergottite meteorites

On the secular retention of ground water and ice on Mars

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