Experimental petrology of the basaltic shergottite Yamato-980459: Implications for the thermal structure of the Martian mantle

White, Donald S. Mussel; Dalton, H.; Kiefer, W. S.; Treiman, Allan H.

doi:10.1111/j.1945-5100.2006.tb00521.x

Cited by 131 publications

(33 citation statements)

References 52 publications

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“…Initial calculations were conducted on four proposed parental melt compositions. For the Yamato 980459 shergottite (hereafter Y-98), we used the bulk rock composition [Musselwhite et al, 2006], and for shergottites LAR 06319 and NWA 1068 we used compositions corrected for olivine fractionation and mixing [Filiberto et al, 2010;. We also included a proposed parental Gusev crater basalt composition analyzed by the Spirit rover [McSween et al, 2006].…”

Section: Methodsmentioning

confidence: 99%

“…However, it rapidly became clear as discussed below that the MELTS calibration calculations were unable to fit the pressure of the olivine-pyroxene multiple-saturation point, the single pressure where both olivine and a pyroxene are simultaneously on the liquidus. As this point is the best available single point for comparison between experiments and calculations at elevated pressures and has been used as a proxy for the last depth of equilibration between Martian magmas and the mantle [e.g., Musselwhite et al, 2006;Filiberto et al, 2010], this lack of agreement posed a major difficulty. However, we noted that many Martian multiplesaturation pressures were within the range of pressures where the pMELTS calibration could be applicable, and previous authors have used pMELTS calibration calculations to analyze multiple saturation in terrestrial magmas [Asimow and Longhi, 2004].…”

Section: Methodsmentioning

confidence: 99%

“…[14] These choices of pressures, volatile contents, and redox conditions were meant to cover the range of plausible crystallization conditions on Mars, from beneath the crust [e.g., Wieczorek and Zuber, 2004;Musselwhite et al, 2006;Filiberto et al, 2010] to the surface and from dry to moderately hydrous magmas. Previous authors have argued that Martian parental magmas may contain up to~2 wt.…”

Section: Methodsmentioning

confidence: 99%

“…[6] Continued discovery of new Martian meteorites and analyses of rocks by rovers on Mars have produced a wealth of new igneous compositions in the years since the MELTS and pMELTS calibrations were published. Furthermore, there have been multiple estimates of Martian parental magma compositions [e.g., Musselwhite et al, 2006;McSween et al, 2006;Monders et al, 2007;Gross et al, 2011;Filiberto et al, 2010;Filiberto and Dasgputa, 2011;Basu Sarbadhikari et al, 2011; and experimental studies of magma crystallization [Musselwhite et al, 2006;Monders et al, 2007;Filiberto et al, 2008;McCubbin et al, 2008;Filiberto and Treiman, 2009b;Filiberto et al, 2010]. These studies provide motivation to evaluate the applicability of the MELTS algorithm to Mars in a new way; rather than evaluating individual crystallization scenarios, we can compare MELTS calculations to the actual crystallization paths and compositions of Martian basalts in aggregate.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Balta

McSween

2013

JGR Planets

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“…An exception is the olivine-phyric shergottite Yamato 980459 (Y980459), which has been extensively studied due to its vitrophyric groundmass texture indicative of rapid cooling, and a whole-rock composition that has been interpreted as a relatively primitive melt of the Martian mantle (First & Hammer, 2016;Greshake et al, 2004;Musselwhite et al, 2006;Usui et al, 2008). Thin sections of Y980459 have relatively large (up to~100 μm longest dimension) glassy magmatic inclusions contained in olivine (Greshake et al, 2004;Ikeda, 2004;Ikeda, 2005).…”

Section: Marsmentioning

confidence: 99%

Controlled Cooling‐Rate Experiments on Olivine‐Hosted Melt Inclusions: Chemical Diffusion and Quantification of Eruptive Cooling Rates on Hawaii and Mars

Saper

Stolper

2020

Geochem Geophys Geosyst

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Controlled cooling‐rate experiments were conducted on olivine‐hosted melt inclusions to characterize the development of compositional zoning observed in natural inclusions. All of the experimentally cooled inclusions are zoned due to olivine crystallization on the inclusion wall and diffusive exchange between the boundary layer adjacent to the growing olivine and the inclusion centers. Experimentally cooled inclusions are characterized by lower MgO and FeO and higher SiO2, Al2O3, and Na2O (and other incompatible oxides) near the inclusion wall relative to the inclusion center. The compositions at the centers of inclusions are susceptible to modification by diffusion, particularly for small inclusions and those subjected to low cooling rates. Uphill diffusion is evident in every oxide and is recognized by local extrema along a diffusion profile. CaO exhibits the most extreme manifestation of uphill diffusion, and a model attributes the diffusion behavior in CaO to solution nonideality in the boundary layer liquid. MgO profiles from experimentally cooled inclusions were fit with a diffusion model by varying the cooling rate. The cooling rates that resulted in the best fit models were always within a factor of 2 and typically within ±10% of the experimental cooling rates, which ranged from 70 to 50,000 °C/hr. The model was applied to MgO profiles across natural glassy olivine‐hosted melt inclusions from Hawaii and the shergottite Yamato 980459. Cooling rates from zoned melt inclusions in Yamato 980459 range from 85 to 1,047 °C/hr (mean = 383±43 °C/hr, 1σ, n=8) and support the hypothesis that the sample erupted at or near the Martian surface.

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Exploring fractionation models for Martian magmas

2014

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[1] Martian primary compositions, i.e., magmas that did not experience fractionation and/or contamination after extraction from the mantle, occur as a subset of Martian meteorites and a few lavas analyzed on the planet's surface by rovers. Eruptions of primary magmas are rare on Earth and presumably on Mars. Previous studies of fractional crystallization of Martian primary magmas have been conducted under isobaric conditions, simulating idealized crystallization in magma chambers. Polybaric fractionation, which occurs during magma ascent, has not been investigated in detail for Martian magmas. Using the MELTS algorithm and the pMELTS revision, we present comprehensive isobaric and polybaric thermodynamic calculations of the fractional crystallization of four primary or parental Martian magmas (Humphrey, Fastball, Y-980459 shergottite, and nakhlite parental melts) using various pressure-temperature paths, oxygen fugacities, and water contents to constrain how these magmas might evolve. We then examine whether known Martian alkaline rock compositions could have formed through fractional crystallization of these magmas under the simulated conditions. We find that isobaric and polybaric crystallization paths produce similar residual melt compositions, but given sufficient details, we may be able to distinguish between them. We calculate that Backstay (Gusev Crater) likely formed by fractionation of a primary magma under polybaric conditions, while Jake_M (Gale Crater) may have formed through melting of a metasomatized mantle, crustal assimilation, or fractional crystallization of an unknown primary magma. The best fits for the Backstay composition indicate that consideration of polybaric crystallization paths can help improve the quality of fit when simulating liquid lines of descent.

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Experimental petrology of the basaltic shergottite Yamato-980459: Implications for the thermal structure of the Martian mantle

Cited by 131 publications

References 52 publications

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

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

Controlled Cooling‐Rate Experiments on Olivine‐Hosted Melt Inclusions: Chemical Diffusion and Quantification of Eruptive Cooling Rates on Hawaii and Mars

Exploring fractionation models for Martian magmas

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