Syneruptive incorporation of martian surface sulphur in the nakhlite lava flows revealed by S and Os isotopes and highly siderophile elements: implication for mantle sources in Mars

Mari, Nicola; Riches, Amy; Hallis, L. J.; Marrocchi, Yves; Villeneuve, Johan; Gleißner, Philipp; Becker, Harry; Lee, Martin

doi:10.1016/j.gca.2019.05.025

Cited by 12 publications

(26 citation statements)

References 97 publications

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“…Similarly, the high sulfide content, coupled with Ni-free pyrrhotite compositions in CeC 022, also resembles MIL's nakhlites (Day et al 2006;Franz et al 2014;Dottin et al 2018). Assimilation of crustal sulfur during the igneous crystallization stage could account for CeC 022 pyrrhotite modal abundance and Ni-poor composition, as repeatedly documented in nakhlites, especially in the fast-cooled subgroup (Farquhar et al 2007;Franz et al 2014Franz et al , 2019Dottin et al 2018;Mari et al [2019] and reference therein). The mean Fe/S ratio of CeC 022 pyrrhotite (Fe 0.89 S; hexagonal pyrrhotite) ( Fig.…”

Section: Sulfidessupporting

confidence: 53%

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Caleta el Cobre 022 Martian meteorite: Increasing nakhlite diversity

Ruggiu

Gattacceca

Devouard

et al. 2020

Meteorit & Planetary Scien

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Caleta el Cobre (CeC) 022 is a Martian meteorite of the nakhlite group, showing an unbrecciated cumulate texture, composed mainly of clinopyroxene and olivine. Augite shows irregular core zoning, euhedral rims, and thin overgrowths enriched in Fe relative to the core. Low‐Ca pyroxene is found adjacent to olivine. Phenocrysts of Fe‐Ti oxides are titanomagnetite with exsolutions of ilmenite/ulvöspinel. Intercumulus material consists of both coarse plagioclase and fine‐grained mesostasis, comprising K‐feldspars, pyroxene, apatite, ilmenite, Fe‐Ti oxides, and silica. CeC 022 shows a high proportion of Martian aqueous alteration products (iddingsite) in olivine (45.1 vol% of olivine) and mesostasis. This meteorite is the youngest nakhlite with a distinct Sm/Nd crystallization age of 1.215 ± 0.067 Ga. Its ejection age of 11.8 ± 1.8 Ma is similar to other nakhlites. CeC 022 reveals contrasted cooling rates with similarities with faster cooled nakhlites, such as Northwest Africa (NWA) 817, NWA 5790, or Miller Range 03346 nakhlites: augite irregular cores, Fe‐rich overgrowths, fine‐grained K‐feldspars, quenched oxides, and high rare earth element content. CeC 022 also shares similarities with slower cooled nakhlites, including Nakhla and NWA 10153: pyroxene modal abundance, pyroxenes crystal size distribution, average pyroxene size, phenocryst mineral compositions, unzoned olivine, and abundant coarse plagioclase. Moreover, CeC 022 is the most magnetic nakhlite and represents an analog source lithology for the strong magnetization of the Martian crust. With its particular features, CeC 022 must originate from a previously unsampled sill or flow in the same volcanic system as the other nakhlites, increasing Martian sample diversity and our knowledge of nakhlites.

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Section: Sulfidessupporting

confidence: 53%

“…Caleta el Cobre 022 is sulfide-rich (0.15 AE 0.05 vol%) compared to other nakhlites so far studied for sulfides (Chevrier et al 2011;Franz et al 2014;Dottin et al 2018;Mari et al 2019).…”

Section: Sulfidesmentioning

confidence: 91%

Caleta el Cobre 022 Martian meteorite: Increasing nakhlite diversity

Ruggiu

Gattacceca

Devouard

et al. 2020

Meteorit & Planetary Scien

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“…2018; Franz 2019a, 2019b; Mari et al. 2019). Ni‐bearing pyrrhotite (3 wt% Ni) + pentlandite was identified only as three inclusions in plagioclase clasts over the eight polished thick sections investigated.…”

Section: Sulfide Mineralogy Of Nwa 7533mentioning

confidence: 99%

“…2011; Mari et al. 2019). The nakhlite meteorites which contain both sulfate and magmatic sulfide minerals display the largest range of MIF anomalies (Farquhar et al.…”

Section: Introductionmentioning

confidence: 99%

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The sulfur budget and sulfur isotopic composition of Martian regolith breccia NWA 7533

Lorand

Labidi

Rollion‐Bard

et al. 2020

Meteorit & Planetary Scien

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The sulfur isotope budget of Martian regolith breccia (NWA 7533) has been addressed from conventional fluorination bulk rock analyses and ion microprobe in situ analyses. The bulk rock analyses yield 865 AE 50 ppm S in agreement with LA-ICP-MS analyses. These new data support previous estimates of 80% S loss resulting from terrestrial weathering of NWA 7533 pyrite. Pyrite is by far the major S host. Apatite and Fe oxyhydroxides are negligible S carriers, as are the few tiny igneous pyrrhotite-pentlandite sulfide grains included in lithic clasts so far identified. A small nonzero D 33 S (À0.029 AE 0.010&) signal is clearly resolved at the 2r level in the bulk rock analyses, coupled with negative CDT-normalized d 34 S (À2.54 AE 0.10&), and near-zero D 36 S (0.002 AE 0.09&). In situ analyses also yield negative D 33 S values (À0.05 to À0.30&) with only a few positive D 33 S up to +0.38&. The slight discrepancy compared to the bulk rock results is attributed to a possible sampling bias. The occurrence of mass-independent fractionation (MIF) supports a model of NWA 7533 pyrite formation from surface sulfur that experienced photochemical reaction(s). The driving force that recycled crustal S in NWA 7533 lithologies-magmatic intrusions or impact-induced heat-is presently unclear. However, in situ analyses also gave negative d 34 S values (+1 to À5.8&). Such negative values in the hydrothermal setting of NWA 7533 are reflective of hydrothermal sulfides precipitated from H 2 S/HSaqueous fluid produced via open-system thermochemical reduction of sulfates at high temperatures (>300°C).

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