Petrology of igneous clasts in Northwest Africa 7034: Implications for the petrologic diversity of the martian crust

Santos, A. R.; Agee, C. B.; McCubbin, F. M.; Shearer, C. K.; Burger, P. V.; Tartèse, Romain; Anand, M.

doi:10.1016/j.gca.2015.02.023

Cited by 113 publications

(224 citation statements)

References 101 publications

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“…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.%). Other components of NWA 7034 exhibit low CaO/Al 2 O 3 (∼0.5) ratios for relatively high MgO contents compared to experimental melts .…”

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

confidence: 63%

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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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: 63%

“…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). The TiO 2 content (2.3 wt.%) is out of the field.…”

Section: Columbia Hills: Alkali Basaltsmentioning

confidence: 99%

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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“…Data from lunar samples were compiled from the Lunar Sample Compendium. Data from Mars were compiled from the Mars Meteorite Compendium as well as data from Aoudjehane et al () and Santos et al (). Data from terrestrial rocks were downloaded from the PetDB (Lehnert et al, ) database ( www.earthchem.org/petdb) on 8 September, 2017, using the following parameters: Data availability = major oxides and sample type = igneous:volcanic:mafic.…”

Section: O/si Ratio From Messenger Grsmentioning

confidence: 99%

A Low O/Si Ratio on the Surface of Mercury: Evidence for Silicon Smelting?

et al. 2017

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Data from the Gamma‐Ray Spectrometer (GRS) that flew on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft indicate that the O/Si weight ratio of Mercury's surface is 1.2 ± 0.1. This value is lower than any other celestial surface that has been measured by GRS and suggests that 12–20% of the surface materials on Mercury are composed of Si‐rich, Si‐Fe alloys. The origin of the metal is best explained by a combination of space weathering and graphite‐induced smelting. The smelting process would have been facilitated by interaction of graphite with boninitic and komatiitic parental liquids. Graphite entrained at depth would have reacted with FeO components dissolved in silicate melt, resulting in the production of up to 0.4–0.9 wt % CO from the reduction of FeO to Fe0—CO production that could have facilitated explosive volcanic processes on Mercury. Once the graphite‐entrained magmas erupted, the tenuous atmosphere on Mercury prevented the buildup of CO over the lavas. The partial pressure of CO would have been sufficiently low to facilitate reaction between graphite and SiO2 components in silicate melts to produce CO and metallic Si. Although exotic, Si‐rich metal as a primary smelting product is hypothesized on Mercury for three primary reasons: (1) low FeO abundances of parental magmas, (2) elevated abundances of graphite in the crust and regolith, and (3) the presence of only a tenuous atmosphere at the surface of the planet within the 3.5–4.1 Ga timespan over which the planet was resurfaced through volcanic processes.

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“…; Santos et al. ). There is also substantial diversity among the igneous clast types, including basalts, basaltic andesites, and trachyandesites (Humayun et al.…”

Section: Introductionmentioning

confidence: 98%

“…; Santos et al. ), although it has also been called a regolith breccia (Muttik et al. ; Wittmann et al.…”

Section: Introductionmentioning

confidence: 99%

Rb‐Sr and Sm‐Nd isotopic and REE studies of igneous components in the bulk matrix domain of Martian breccia Northwest Africa 7034

Nyquist

Shih

McCubbin

et al. 2016

Meteorit & Planetary Scien

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Petrology of igneous clasts in Northwest Africa 7034: Implications for the petrologic diversity of the martian crust

Cited by 113 publications

References 101 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

A Low O/Si Ratio on the Surface of Mercury: Evidence for Silicon Smelting?

Rb‐Sr and Sm‐Nd isotopic and REE studies of igneous components in the bulk matrix domain of Martian breccia Northwest Africa 7034

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