Experimental and crystal chemical study of the basalt–eclogite transition in Mars and implications for martian magmatism

Papike, J. J.; Burger, P. V.; Shearer, C. K.; McCubbin, F. M.

doi:10.1016/j.gca.2012.11.007

Cited by 16 publications

(16 citation statements)

References 68 publications

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“…For example, a potassic metasomatic fluid could be mobilized from eclogite (e.g., pressure > ~1.5 GPa) or plagioclase peridotite (pressure < ~1 GPa), with Na 2 O being retained in the residue in omphacitic pyroxene or plagioclase, respectively (e.g., Papike et al. ), while K 2 O is concentrated in the melt and fluid (e.g., Keshav et al. ).…”

Section: Discussionmentioning

confidence: 99%

“…Potassic metasomatism resulting in Na 2 O/K 2 O fractionation occurs in the Earth's mantle, as evidenced by xenoliths with veins rich in biotite and K-amphibole (O'Reilly and Griffin 2013) and by potassic basalts (Elkins-Tanton and Grove 2003). For example, a potassic metasomatic fluid could be mobilized from eclogite (e.g., pressure >~1.5 GPa) or plagioclase peridotite (pressure <~1 GPa), with Na 2 O being retained in the residue in omphacitic pyroxene or plagioclase, respectively (e.g., Papike et al 2013), while K 2 O is concentrated in the melt and fluid (e.g., Keshav et al 2004).…”

Section: Generation Of K 2 O-rich Melt and Implications For Differentmentioning

confidence: 99%

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K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

Goodrich

Treiman

Filiberto

et al. 2013

Meteorit & Planetary Scien

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Abstract-We used new analytical and theoretical methods to determine the major and minor element compositions of the primary trapped liquid (PTLs) represented by melt inclusions in olivine and augite in the Martian clinopyroxenite, Nakhla, for comparison with previously proposed compositions for the Nakhla (or nakhlite) parent magma. We particularly focused on obtaining accurate K 2 O contents, and on testing whether high K 2 O contents and K 2 O/ Na 2 O ratios obtained in previous studies of melt inclusions in olivine in Nakhla could have been due to unrepresentative sampling, systematic errors arising from electron microprobe techniques, late alteration of the inclusions, and/or boundary layer effects. Based on analyses of 35 melt inclusions in olivine cores, the PTL in olivine, PTL oliv , contained (by wt) approximately 47% SiO 2 , 6.3% Al 2 O 3 , 9.6% CaO, 1.8% K 2 O, and 0.9% Na 2 O, with K 2 O/ Na 2 O = 2.0. We infer that the high K 2 O content of PTL oliv is not due to boundary layer effects and represents a real property of the melt from which the host olivine crystallized. This melt was cosaturated with olivine and augite. Its mg# is model-dependent and is constrained only to be ≥19 (equilibrium Fo = 40). Based on analyses of 91 melt inclusions in augite cores, the PTL in augite, PTL aug , contained (by wt) 53-54% SiO 2 , 7-8% Al 2 O 3 , 0.8-1.1% K 2 O, and 1.1-1.4% Na 2 O, with K 2 O/Na 2 O = 0.7-0.8. This K 2 O content and K 2 O/Na 2 O ratio are significantly higher than inferred in studies of melt inclusions in augite in Nakhla by experimental rehomogenization. PTL aug was saturated only with augite, and in equilibrium with augite cores of mg# 62. PTL aug represents the Nakhla parent magma, and does not evolve to PTL oliv by fractional crystallization. We therefore conclude that olivine cores in Nakhla (and, by extension, other nakhlites) are xenocrystic. We propose that PTL oliv and PTL aug were generated from the same source region. PTL oliv was generated first and emplaced to form olivine-rich cumulate rocks. Shortly thereafter, PTL aug was generated and ascended through these olivine-rich cumulates, incorporating fragments of wallrock that became the xenocrystic olivine cores in Nakhla. The Nakhla (nakhlite) mantle source region was pyroxenitic with some olivine, and could have become enriched in K relative to Na via metasomatism. A high degree of melting of this source produced the silica-poor, alkali-rich magma PTL oliv . Further ascension and decompression of the source led to generation of the silica-rich, relatively alkali-poor magma PTL aug . Potassium-rich magmas like those involved in the formation of the nakhlites represent an important part of the diversity of Martian igneous rocks.

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Section: Discussionmentioning

confidence: 99%

Section: Generation Of K 2 O-rich Melt and Implications For Differentmentioning

confidence: 99%

K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

Goodrich

Treiman

Filiberto

et al. 2013

Meteorit & Planetary Scien

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“…The transition consists in the progressive consumption of plagioclase and appearance of garnet. The transition may start near 50 km to 70 km [Babeyko and Zharkov, 2000;Papike et al, 2013]. Numerical models of the thermochemical evolution of Mars often predict crustal thicknesses significantly above this value (up to 200 km) offering favorable conditions for crustal delamination [e.g., Breuer and Spohn, 2006;Keller and Tackley, 2009].…”

Section: Implication For the Recycling Of The Martian Crustmentioning

confidence: 99%

Petrological constraints on the density of the Martian crust

Baratoux

Samuel

Michaut

et al. 2014

J. Geophys. Res. Planets

100

121

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New insights into the chemistry of the Martian crust have been made available since the derivation of crustal thickness maps from Mars Global Surveyor gravity and topography data that used a conservative range of density values (2700-3100 kg/m 3 ). A new range of crustal density values is calculated from the major element chemistry of Martian meteorites (3100-3700 kg/m 3 ), igneous rocks at Gusev crater (3100-3600 kg/m 3 ) and from the surface concentration of Fe, Al, Ca, Si, and K measured by the Gamma-Ray Spectrometer on board Mars Odyssey (3250-3450 kg/m 3 ). In addition, the density of mineral assemblages resulting from low-pressure crystallization of primary melts of the primitive mantle are estimated for plausible conditions of partial melting corresponding to the Noachian to Amazonian periods (3100-3300 kg/m 3 ). Despite the differences between these approaches, the results are all consistent with an average density above 3100 kg/m 3 for those materials that are close to the surface. The density may be compatible with the measured mass of Mars and the moment of inertia factor, but only if the average crustal thickness is thicker than previously thought (approaching 100 km). A thicker crust implies that crustal delamination and recycling could be possible and may even control its thickness, globally or locally. Alternatively, and considering that geoid-to-topography ratios argue against such a thick crust for the highlands, our results suggest the existence of a buried felsic or anorthositic component in the southern hemisphere of Mars.

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“…Papike et al . [] hypothesized that pyroxene‐rich or eclogite bodies could contribute to Martian magmatism despite the lack of subduction. If such bodies do exist, stagnation at the bottom of the crust followed by delamination is a likely mechanism for generating that type of heterogeneity.…”

Section: Applications Of Our Database Of Melts Calculationsmentioning

confidence: 99%

“…The negative buoyancy of eclogitic cumulates could impose a limit on the allowable thickness of the Martian crust; if enough basaltic material were added to the crust to allow the formation of garnet in the lower crust, it would delaminate and sink. Papike et al [2013] hypothesized that pyroxene-rich or eclogite bodies could contribute to Martian magmatism despite the lack of subduction. If such bodies do exist, stagnation at the bottom of the crust followed by delamination is a likely mechanism for generating that type of heterogeneity.…”

Section: High-feo Basalts and The Rocks Of Gale Cratermentioning

confidence: 99%

Application of the MELTS algorithm to Martian compositions and implications for magma crystallization

Balta

McSween

2013

JGR Planets

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[1] The MELTS algorithm, the most commonly used tool for calculating crystallization of basaltic magmas, uses thermodynamic parameters calibrated by experiments on select compositions, and thus, its use on newly discovered extraterrestrial compositions requires extrapolation across ranges where its applicability has not been evaluated in detail. To apply MELTS to Martian compositions, we undertook a systematic examination of the original MELTS calibration and the pMELTS revision as applied to Martian magmas. We find that the algorithm is effective in predicting the crystallization paths and conditions of Martian magmas, with some issues. The algorithm consistently overestimates the stability of spinel and underestimates pressures of multiple saturation compared to experiments. The pMELTS calibration comes close to fitting multiple-saturation pressures but cannot be used at low pressures. Both calibrations model crystallization temperatures with similar variances to those observed for terrestrial compositions. Both calibrations reproduce important compositional details of crystallizing magmas and coexisting minerals with errors similar to those observed on terrestrial compositions. We calculate several crystallization paths which predict high-FeO, high-density magma compositions that could be a mechanism for cumulate formation. Low-FeO compositions in recent Mars volcanism may be an expression of this density barrier. However, the composition of a high-FeO rock called "Et-Then" discovered by the rover Curiosity is strikingly similar to compositions calculated by the MELTS algorithm and could represent one of these high-FeO volcanic rocks.

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Experimental and crystal chemical study of the basalt–eclogite transition in Mars and implications for martian magmatism

Cited by 16 publications

References 68 publications

K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

Petrological constraints on the density of the Martian crust

Application of the MELTS algorithm to Martian compositions and implications for magma crystallization

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Experimental and crystal chemical study of the basalt–eclogite transition in Mars and implications for martian magmatism

Cited by 16 publications

References 68 publications

K2O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

K2O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

Petrological constraints on the density of the Martian crust

Application of the MELTS algorithm to Martian compositions and implications for magma crystallization

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Product

Resources

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K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle

K₂O‐rich trapped melt in olivine in the Nakhla meteorite: Implications for petrogenesis of nakhlites and evolution of the Martian mantle