Crystallization, melt inclusion, and redox history of a Martian meteorite: Olivine-phyric shergottite Larkman Nunatak 06319

Peslier, A. H.; Hnatyshin, Danny; Herd, Christopher D. K.; Walton, E. L.; Brandon, A. D.; Lapen, T. J.; Shafer, J. T.

doi:10.1016/j.gca.2010.05.002

Cited by 95 publications

(155 citation statements)

References 97 publications

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“…Some shergottites are believed to represent primitive melts (Gross et al, 2013(Gross et al, , 2011Musselwhite et al, 2006;Peslier et al, 2010). However, they exhibit a significant depletion in aluminum when compared to virtually all other analyses of martian rocks (McSween et al, 2009).…”

Section: Shergottites: High Cao/al 2 O 3 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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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: Shergottites: High Cao/al 2 O 3 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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“…However, several researchers (e.g., McSween and Jarosewich, 1983;Wadhwa et al, 2001;Barrat et al, 2002;Filiberto et al, 2010) have interpreted the olivine megacrysts in some olivine -phyric shergottites as exotic xenocrysts or cognate xenocrysts mixed into the olivine -free (or olivine -poor) basaltic magma by other processes. Despite the considerable number of studies conducted regarding the igneous origin of basaltic shergottites, the primitive (parent) magma composition of the Martian mantle remains controversial (e.g., Goodrich, 2002;Greshake et al, 2004;Shearer et al, 2008;Usui et al, 2008;Sarbadhikari et al, 2009;Peslier et al, 2010;Filiberto and Dasgupta, 2011).…”

Section: Introductionmentioning

confidence: 99%

Melting of the Martian mantle from 1.0 to 4.5 GPa

Matsukage

Nagayo

Whitaker

et al. 2013

Journal of Mineralogical and Petrological Sciences

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To investigate the chemical composition of possible primitive melts of the Martian mantle, we performed melting experiments of a model Martian mantle derived by Dreibus and Wänke (DWM) at pressures from 1.0 to 4.5 GPa. The chemical compositions of partial melts are systematically related to pressure. The partial melts at pressure of 1.0 GPa in spinel stability field show high Al 2 O 3 and low FeO contents. The partial melts at higher pressure in garnet stability field are, however, characterized by a relatively high FeO content, low Al 2 O 3 content and high CaO/Al 2 O 3 ratio. In garnet stability field, clinopyroxene (= Ca -rich phase) contribute significantly to melt formation near the solidus temperature, although garnet (= Al -rich phase) is stable at temperature above solidus. Therefore Al -poor and Ca -rich partial melt are formed at higher pressure. Comparing the shergottite chemistry with the chemical trends of the partial melts obtained by the experiments, we suggest that one of basaltic shergottite with a high Al 2 O 3 and low CaO/Al 2 O 3 ratio, QUE94201, resembles the composition of the DWM partial melts in major -element chemistry in a low degree (<20%) partial melt of DWM at pressure of 1.0 GPa and temperature of 1360 °C. We conclude that the olivine -poor (or olivine -free) basaltic magma with low CaO/Al 2 O 3 ratio and high Al 2 O 3 could be primitive melts derived from the upper mantle of Mars if the actual Martian mantle is similar in composition to DWM.

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“…NWA 1068 and LAR 06139 reportedly to show a change in redox state during crystallization (Herd, 2006;Peslier et al, 2010). To examine this possibility, we analyzed the Fe 3+ -Fe 2+ peak-intensity ratios for the core and rim in the same maskelynite grains, which show Fe chemical zoning in LAR 06319 and NWA 4468 (Fig.…”

Section: Fementioning

confidence: 99%

“…However, we did not find any difference between the Fe 3+ -Fe 2+ peak-intensity ratios for the core and rim (NWA 4468 core (NWA 4468-4): 0.68, NWA 4468 rim (NWA 4468-3): 0.68, LAR 06319 core (LAR 06319-2): 0.54, and LAR 06319 rim (LAR 06319-3): 0.56) ( Table. 2). Peslier et al (2010) reported that fO 2 changed during the crystallization of LAR 06319 because the results obtained using the Ol-Px-Sp and Fe-Ti oxide oxybarometers were clearly different. These two oxybarometers recorded fO 2 at high (~1200°C) and low (~900°C) temperatures.…”

Section: Fementioning

confidence: 99%

“…Similarly, ALH 77005 and EETA 79001 lithology A were estimated to have crystallized under an intermediate redox environment (log fO 2 = QFM-2.6 and QFM-2.8 to -1.7), respectively (Herd et al, 2001;Goodrich et al, 2003) (Table 3). The oxygen fugacities of several enriched shergottites were estimated using orthopyroxene-olivine-spinel and Fe-Ti oxide oxybarometers, and the oxygen fugacities were high (LAR 06319: log fO 2 = QFM-2.0 to 0.5, NWA 1068: log fO 2 = QFM-2.5 to -0.5, Zagami: log fO 2 = QFM-1.2, and Shergotty: log fO 2 = QFM-1.2) (Herd et al, 2001;Herd, 2006;Peslier et al, 2010) (Table 3).…”

Section: Fementioning

confidence: 99%

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Redox states of thirteen shergottites as inferred from iron micro X-ray absorption near edge structure of maskelynite

2014

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Crystallization, melt inclusion, and redox history of a Martian meteorite: Olivine-phyric shergottite Larkman Nunatak 06319

Cited by 95 publications

References 97 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

Melting of the Martian mantle from 1.0 to 4.5 GPa

Redox states of thirteen shergottites as inferred from iron micro X-ray absorption near edge structure of maskelynite

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