Petrogenesis of a vitrophyre in the martian meteorite breccia NWA 7034

Udry, Arya; Lunning, N. G.; McSween, H. Y.; Bodnar, Robert J.

doi:10.1016/j.gca.2014.06.026

Cited by 43 publications

(64 citation statements)

References 50 publications

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“…In particular, unlike alkali basalts from Columbia Hills, they are not depleted in CaO and have lower K 2 O/Na 2 O ratios. A vitrophyric clast in NWA 7034 is closer in composition to Humphrey (Adirondack-class) and thus to our higher-degree melts (Udry et al, 2014). The average composition of basalt clasts analyzed by Santos et al (2015) is also within experimental trends with the exception of TiO 2 , which is more than twice as abundant (2.3 wt.%).…”

Section: Nwa 7034/7533: Martian Crust-like Meteoritessupporting

confidence: 66%

“…NWA 7034 M and PB correspond to the composition of the Matrix and Proto-Breccia clasts from McCubbin et al (2015). NWA 7034 V is the vitrophyre from Udry et al (2014). NWA BC 7034 is the average of basaltic clasts from Santos et al (2015).…”

Section: Columbia Hills: Alkali Basaltsmentioning

confidence: 99%

“…The complex texture of NWA 7034/7533 and the diversity of its components make it difficult to argue that it represents a primitive melt or even a silicate liquid. The two clasts displaying magmatic textures, the basaltic clast (VI) of Humayun et al (2013) and the vitrophyre of Udry et al (2014), are impact melts contaminated by a CI chondrite as suggested by their high Ni and Ir contents. However, the chondritic contaminant is unlikely to have disturbed the composition in major elements.…”

Section: Nwa 7034/7533: Martian Crust-like Meteoritesmentioning

confidence: 99%

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Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Collinet

Médard

Charlier

et al. 2015

Earth and Planetary Science Letters

109

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We have performed piston-cylinder experiments on a primitive martian mantle composition between 0.5 and 2.2 GPa and 1160 to 1550 • C. The composition of melts and residual minerals constrain the possible melting processes on Mars at 50 to 200 km depth under nominally anhydrous conditions. Silicate melts produced by low degrees of melting (<10 wt.%) were analyzed in layers of vitreous carbon spheres or in micro-cracks inside the graphite capsule. The total range of melt fractions investigated extends from 5 to 50 wt.%, and the liquids produced display variable SiO 2 (43.7-59.0 wt.%), MgO (5.3-18.6 wt.%) and Na 2 O + K 2 O (1.0-6.5 wt.%) contents. We provide a new equation to estimate the solidus temperature of the martian mantle: T ( • C) = 1033 + 168.1P (GPa) − 14.22P 2 (GPa), which places the solidus 50 • C below that of fertile terrestrial peridotites. Low-and high-degree melts are compared to martian alkaline rocks and basalts, respectively. We suggest that the parental melt of Adirondack-class basalts was produced by ∼25 wt.% melting of the primitive martian mantle at 1.5 GPa (∼135 km) and ∼1400 • C. Despite its brecciated nature, NWA 7034/7533 might be composed of material that initially crystallized from a primary melt produced by ∼10-30 wt.% melting at the same pressure. Other igneous rocks from Mars require mantle reservoirs with different CaO/Al 2 O 3 and FeO/MgO ratios or the action of fractional crystallization. Alkaline rocks can be derived from mantle sources with alkali contents (∼0.5 wt.%) similar to the primitive mantle.

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Section: Nwa 7034/7533: Martian Crust-like Meteoritessupporting

confidence: 66%

Section: Columbia Hills: Alkali Basaltsmentioning

confidence: 99%

Section: Nwa 7034/7533: Martian Crust-like Meteoritesmentioning

confidence: 99%

See 1 more Smart Citation

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Collinet

Médard

Charlier

et al. 2015

Earth and Planetary Science Letters

109

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“…Three out of the four rocks show chemical similarities and may be related [ Schmidt et al , ]; the other rock, Jake_M, is a silica‐undersaturated mugearite and potentially unrelated to the other rocks analyzed in Gale Crater [ Stolper et al , ; Schmidt et al , ]. NWA 7034 (and paired stones), a Martain regolith breccia, contains clasts of mugearite and other similarly silca‐ and alkali‐rich compositions [ Agee et al , ; Santos et al , , 2014b; Udry et al , ]. These rocks extend the compositional space to more evolved compositions than exhibited in the meteorite collection or analyzed at any other landing site [ Agee et al , ; Humayun et al , ; Santos et al , ; Stolper et al , ; Schmidt et al , ; Udry et al , ].…”

Section: Introductionmentioning

confidence: 99%

“…NWA 7034 (and paired stones), a Martain regolith breccia, contains clasts of mugearite and other similarly silca‐ and alkali‐rich compositions [ Agee et al , ; Santos et al , , 2014b; Udry et al , ]. These rocks extend the compositional space to more evolved compositions than exhibited in the meteorite collection or analyzed at any other landing site [ Agee et al , ; Humayun et al , ; Santos et al , ; Stolper et al , ; Schmidt et al , ; Udry et al , ]. Therefore, they may represent magmas that tapped a previously unstudied source region ( P and/or T ).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the depth and thermal vigor of melting in the Martian mantle

Filiberto

Dasgupta

2015

JGR Planets

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Studies of rocks in Gale Crater and clasts within the Martian meteorite breccia Northwest Africa (NWA) 7034 (and paired stones) have expanded our knowledge of the diversity of igneous rocks that make up the Martian crust beyond those compositions exhibited in the meteorite collection or analyzed at any other landing site. Therefore, the magmas that gave rise to these rocks may have been generated at significantly different conditions in the Martian mantle than those derived from previously studied rocks. Here we build upon our previous models of basalt formation based on rocks analyzed in Gusev Crater and Meridiani Planum to the new models of basalt formation for compositions from Gale Crater and a clast in meteorite NWA 7034. Estimates for the mantle potential temperature, T P based on Noachian age rock analyses in Gale Crater, Gusev Crater, and Bounce Rock in Meridiani Planum, and a vitrophyre clast in NWA 7034 are within error, which suggests that the calculated average T P of 1450 ± 70°C may represent an average global mantle temperature during the Noachian. The T P estimates for the Hesperian and Amazonian, based on orbital analyses of the chemistry of the crust, are lower in temperature than our estimates for the Noachian, which is consistent with simple convective cooling of the interior of Mars. However, the T P estimates from the young meteorites are significantly higher than the estimates based on surface chemistry and are consistent with localized "hot spot" melting and not heating up of the interior.

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Potassium‐rich sandstones within the Gale impact crater, Mars: The APXS perspective

et al. 2016

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The Alpha Particle X‐ray spectrometer (APXS) on board the Curiosity rover at the Kimberley location within Gale crater, Mars, analyzed basaltic sandstones that are characterized by potassium enrichments of 2 to 8 times estimates for average Martian crust. They are the most potassic rocks sampled on Mars to date. They exhibit elevated Fe, Mg, Mn and Zn and depleted Na, Al, and Si. These compositional characteristics are common to other potassic sedimentary rocks analyzed by APXS at Gale but distinct from other landing sites and Martian meteorites. CheMin and APXS analysis of a drilled sample indicate mineralogy dominated by sanidine, Ca‐rich and Ca‐poor clinopyroxene, magnetite, olivine, and andesine. The anhydrous mineralogy of the Kimberley sample, and the normative mineralogy derived from APXS of other Bathurst class rocks, together indicate provenance from one or more potassium‐rich magmatic or impact‐generated source rocks on the rim of Gale crater or beyond. Elevated Zn, Ge, and Cu suggest that a localized area of the source region(s) experienced hydrothermal alteration, which was subsequently eroded, dispersed, and diluted throughout the unaltered sediment during transport and deposition. The identification of the basaltic, high potassium Bathurst class and other distinct rock compositional classes by the APXS, attests to the diverse chemistry of crustal rocks within and in the vicinity of Gale crater. We conclude that weathering, transport, and diagenesis of the sediment did not occur in a warm and wet environment, but instead under relatively cold and wet conditions, perhaps more fitting with processes typical of glacial/periglacial environments.

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Petrogenesis of a vitrophyre in the martian meteorite breccia NWA 7034

Cited by 43 publications

References 50 publications

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Melting of the primitive martian mantle at 0.5–2.2 GPa and the origin of basalts and alkaline rocks on Mars

Constraints on the depth and thermal vigor of melting in the Martian mantle

Potassium‐rich sandstones within the Gale impact crater, Mars: The APXS perspective

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